2024-03-28T20:54:40Zhttps://scholarworks.iu.edu/dspace-oai/requestoai:scholarworks.iu.edu:2022/133042011-05-25T12:35:28Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Michael, Scott
Durisen, Richard H.
Boley, Aaron C.
2011-05-25T12:35:28Z
2011-05-25T12:35:28Z
2011-05-25T12:35:28Z
http://hdl.handle.net/2022/13304
Characterization of migration in gravitationally unstable disks is necessary to understand the fate of protoplanets formed by disk instability. As part of a larger study, we are using a 3D radiative hydrodynamics code to investigate how an embedded gas giant planet interacts with a gas disk that undergoes gravitational instabilities (GIs). This Letter presents preliminary results from simulations with a Jupiter-mass planet placed in orbit at 25 AU within a 0.14 M_sun disk. The disk spans 5 to 40 AU around a 1 M_sun star and is initially close to marginal stability. In one simulation, the planet is inserted prior to the eruption of GIs; in another, it is inserted only after the disk has settled into a quasi-steady GI-active state, where heating by GIs roughly balances radiative cooling. When the planet is present from the beginning, its own wake stimulates growth of a particular global mode with which it strongly interacts, and the planet plunges inward six AU in about 1000 years. In both cases with embedded planets, there are times when the planet's radial motion is slow and varies in direction. At other times, when the planet appears to be interacting with strong spiral modes, migration both inward and outward can be relatively rapid, covering several AUs over hundreds of years. Migration in both cases appears to stall near the inner Lindblad resonance of a dominant low-order mode. Planet orbit eccentricities fluctuate rapidly between about 0.02 to 0.1 throughout the GI-active phases of the simulations.
Submitted by Scott Michael (scamicha@iu.edu) on 2011-05-24T20:06:47Z
No. of bitstreams: 3
BASELINE.mpg: 48993272 bytes, checksum: c4d9791e16b7e21cd1e76651ed663da9 (MD5)
1JUP10ORP.mpg: 25683207 bytes, checksum: 0b8c800c848f4781ece42243636304c4 (MD5)
1JUP0ORP.mpg: 25934003 bytes, checksum: 8433762e108f9c43d3b58476faab487c (MD5)
Approved for entry into archive by Scott Michael(scamicha@iu.edu) on 2011-05-25T12:35:28Z (GMT) No. of bitstreams: 3
BASELINE.mpg: 48993272 bytes, checksum: c4d9791e16b7e21cd1e76651ed663da9 (MD5)
1JUP10ORP.mpg: 25683207 bytes, checksum: 0b8c800c848f4781ece42243636304c4 (MD5)
1JUP0ORP.mpg: 25934003 bytes, checksum: 8433762e108f9c43d3b58476faab487c (MD5)
Made available in DSpace on 2011-05-25T12:35:28Z (GMT). No. of bitstreams: 3
BASELINE.mpg: 48993272 bytes, checksum: c4d9791e16b7e21cd1e76651ed663da9 (MD5)
1JUP10ORP.mpg: 25683207 bytes, checksum: 0b8c800c848f4781ece42243636304c4 (MD5)
1JUP0ORP.mpg: 25934003 bytes, checksum: 8433762e108f9c43d3b58476faab487c (MD5)
en
protoplanetary disks
planets and satellites: formation
planet-disk interactions
instabilities
hydrodynamics
Migration of Gas Giant Planets in Gravitationally Unstable Disks
Article
ORIGINAL
1JUP0ORP.mpg
1JUP0ORP.mpg
The t=0 run
video/mpeg
25934003
https://scholarworks.iu.edu/dspace/bitstream/2022/13304/1/1JUP0ORP.mpg
8433762e108f9c43d3b58476faab487c
MD5
1
1JUP10ORP.mpg
1JUP10ORP.mpg
The t=10 run
video/mpeg
25683207
https://scholarworks.iu.edu/dspace/bitstream/2022/13304/2/1JUP10ORP.mpg
0b8c800c848f4781ece42243636304c4
MD5
2
BASELINE.mpg
BASELINE.mpg
The fiducial run
video/mpeg
48993272
https://scholarworks.iu.edu/dspace/bitstream/2022/13304/3/BASELINE.mpg
c4d9791e16b7e21cd1e76651ed663da9
MD5
3
LICENSE
license.txt
license.txt
text/plain
2049
https://scholarworks.iu.edu/dspace/bitstream/2022/13304/4/license.txt
3041a2fa4bfc42705001e572594504ce
MD5
4
2022/13304
oai:scholarworks.iu.edu:2022/13304
2011-05-25 08:35:28.766
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190452021-10-18T13:39:09Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Yong, D.
Carney, B.W.
Friel, E.D.
2014-10-22T18:41:49Z
2014-10-22T18:41:49Z
2012
Yong, D., Carney, B. W., & Friel, E. D. (2012). Elemental abundance ratios in stars of the outer galactic disk. IV. A new sample of open clusters. Astronomical Journal, 144(4), 95. http://dx.doi.org/10.1088/0004-6256/144/4/95
http://hdl.handle.net/2022/19045
We present radial velocities and chemical abundances for nine stars in the old, distant open clusters Be18, Be21, Be22, Be32, and PWM4. For Be18 and PWM4, these are the first chemical abundance measurements. Combining our data with literature results produces a compilation of some 68 chemical abundance measurements in 49 unique clusters. For this combined sample, we study the chemical abundances of open clusters as a function of distance, age, and metallicity. We confirm that the metallicity gradient in the outer disk is flatter than the gradient in the vicinity of the solar neighborhood. We also confirm that the open clusters in the outer disk are metal-poor with enhancements in the ratios [$\alpha$/Fe] and perhaps [Eu/Fe]. All elements show negligible or small trends between [X/Fe] and distance (<0.02dexkpc$^{-1}$), but for some elements, there is a hint that the local (R$_{GC}$< 13kpc) and distant (R$_{GC}$> 13kpc) samples may have different trends with distance. There is no evidence for significant abundance trends versus age (<0.04dex Gyr$^{-1}$). We measure the linear relation between [X/Fe] and metallicity, [Fe/H], and find that the scatter about the mean trend is comparable to the measurement uncertainties. Comparison with solar neighborhood field giants shows that the open clusters share similar abundance ratios [X/Fe] at a given metallicity. While the flattening of the metallicity gradient and enhanced [$\alpha$/Fe] ratios in the outer disk suggest a chemical enrichment history different from that of the solar neighborhood, we echo the sentiments expressed by Friel etal. that definitive conclusions await homogeneous analyses of larger samples of stars in larger numbers of clusters. Arguably, our understanding of the evolution of the outer disk from open clusters is currently limited by systematic abundance differences between various studies.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-22T18:41:15Z
No. of bitstreams: 1
1538-3881_144_4_95.pdf: 3730292 bytes, checksum: ef4b1b4e24da5fcdb0ee5c9060b4be8d (MD5)
Approved for entry into archive by Shayna Pekala (spekala@indiana.edu) on 2014-10-22T18:41:49Z (GMT) No. of bitstreams: 1
1538-3881_144_4_95.pdf: 3730292 bytes, checksum: ef4b1b4e24da5fcdb0ee5c9060b4be8d (MD5)
Made available in DSpace on 2014-10-22T18:41:49Z (GMT). No. of bitstreams: 1
1538-3881_144_4_95.pdf: 3730292 bytes, checksum: ef4b1b4e24da5fcdb0ee5c9060b4be8d (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-6256/144/4/95
© 2012 The American Astronomical Society
Galaxy: abundances
Galaxy: disk
open clusters and associations: general
Elemental abundance ratios in stars of the outer galactic disk. IV. A new sample of open clusters
Article
false
ORIGINAL
1538-3881_144_4_95.pdf
1538-3881_144_4_95.pdf
application/pdf
3730292
https://scholarworks.iu.edu/dspace/bitstream/2022/19045/1/1538-3881_144_4_95.pdf
ef4b1b4e24da5fcdb0ee5c9060b4be8d
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19045/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
friel_eileen_license_2012.txt
friel_eileen_license_2012.txt
text/plain
4514
https://scholarworks.iu.edu/dspace/bitstream/2022/19045/3/friel_eileen_license_2012.txt
7f67dc26373d0ba462ad32a5cd275b09
MD5
3
TEXT
1538-3881_144_4_95.pdf.txt
1538-3881_144_4_95.pdf.txt
Extracted text
text/plain
117143
https://scholarworks.iu.edu/dspace/bitstream/2022/19045/4/1538-3881_144_4_95.pdf.txt
878b7b1e17397269ae98d2ffff537a91
MD5
4
THUMBNAIL
1538-3881_144_4_95.pdf.jpg
1538-3881_144_4_95.pdf.jpg
IM Thumbnail
image/jpeg
3824
https://scholarworks.iu.edu/dspace/bitstream/2022/19045/5/1538-3881_144_4_95.pdf.jpg
3545c370332673f439df48e2c04750d4
MD5
5
2022/19045
oai:scholarworks.iu.edu:2022/19045
2021-10-18 09:39:09.11
IUScholarWorks
iusw@indiana.edu
CkJ5IHNpZ25pbmcgYW5kIHN1Ym1pdHRpbmcgdGhpcyBsaWNlbnNlLCB5b3UgKHRoZSBjcmVhdG9yIG9yIGNvcHlyaWdodCBvd25lcikgZ3JhbnQgdG8gSW5kaWFuYSBVbml2ZXJzaXR5IGEgbm9uLWV4Y2x1c2l2ZSwgcGVycGV0dWFsLCBpcnJldm9jYWJsZSByaWdodCB0byByZXByb2R1Y2UsIHRyYW5zbGF0ZSAoYXMgZGVmaW5lZCBiZWxvdyksIGFuZC9vciBkaXN0cmlidXRlIHlvdXIgc3VibWlzc2lvbiAoaW5jbHVkaW5nIHRoZSBhYnN0cmFjdCkgd29ybGR3aWRlIGluIHByaW50IGFuZCBlbGVjdHJvbmljIGZvcm1hdCBhbmQgaW4gYW55IG1lZGl1bSwgaW5jbHVkaW5nIGJ1dCBub3QgbGltaXRlZCB0byBhdWRpbyBvciB2aWRlby4KCllvdSBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXksIHdpdGhvdXQgY2hhbmdpbmcgdGhlIGNvbnRlbnQsIHRyYW5zbGF0ZSB0aGUgc3VibWlzc2lvbiB0byBhbnkgbWVkaXVtIG9yIGZvcm1hdCBmb3IgcHJlc2VydmF0aW9uIG9yIGFjY2VzcywgYW5kIHByb3ZpZGUgYmFzaWMgbWV0YWRhdGEgdGhhdCBkZXNjcmliZXMgdGhlIGNvbnRlbnRzIGZvciBkaXNjb3ZlcnkuCgpZb3UgYWxzbyBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXkga2VlcCBtb3JlIHRoYW4gb25lIGNvcHkgb2YgdGhpcyBzdWJtaXNzaW9uIGZvciBzZWN1cml0eSwgYmFjay11cCBhbmQgcHJlc2VydmF0aW9uLgoKWW91IHJlcHJlc2VudCB0aGF0IHRoZSBzdWJtaXNzaW9uIGlzIHlvdXIgb3JpZ2luYWwgd29yaywgYW5kIHRoYXQgeW91IGhhdmUgdGhlIHJpZ2h0IHRvIGdyYW50IHRoZSByaWdodHMgY29udGFpbmVkIGluIHRoaXMgbGljZW5zZS4gWW91IGFsc28gcmVwcmVzZW50IHRoYXQgeW91ciBzdWJtaXNzaW9uIGRvZXMgbm90LCB0byB0aGUgYmVzdCBvZiB5b3VyIGtub3dsZWRnZSwgaW5mcmluZ2UgdXBvbiBhbnlvbmUncyBjb3B5cmlnaHQuCgpJZiB0aGUgc3VibWlzc2lvbiBjb250YWlucyBtYXRlcmlhbCBmb3Igd2hpY2ggeW91IGRvIG5vdCBob2xkIGNvcHlyaWdodCwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIG9idGFpbmVkIHRoZSB1bnJlc3RyaWN0ZWQgcGVybWlzc2lvbiBvZiB0aGUgY29weXJpZ2h0IG93bmVyIHRvIGdyYW50IEluZGlhbmEgVW5pdmVyc2l0eSB0aGUgcmlnaHRzIHJlcXVpcmVkIGJ5IHRoaXMgbGljZW5zZSwgYW5kIHRoYXQgc3VjaCB0aGlyZC1wYXJ0eSBvd25lZCBtYXRlcmlhbCBpcyBjbGVhcmx5IGlkZW50aWZpZWQgYW5kIGFja25vd2xlZGdlZCB3aXRoaW4gdGhlIHRleHQgb3IgY29udGVudCBvZiB0aGUgc3VibWlzc2lvbi4KCklmIHRoZSBzdWJtaXNzaW9uIGlzIGJhc2VkIHVwb24gd29yayB0aGF0IGhhcyBiZWVuIHNwb25zb3JlZCBvciBzdXBwb3J0ZWQgYnkgYW4gYWdlbmN5IG9yIG9yZ2FuaXphdGlvbiBvdGhlciB0aGFuIEluZGlhbmEgVW5pdmVyc2l0eSwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIGZ1bGZpbGxlZCBhbnkgcmlnaHQgb2YgcmV2aWV3IG9yIG90aGVyIG9ibGlnYXRpb25zIHJlcXVpcmVkIGJ5IHN1Y2ggY29udHJhY3Qgb3IgYWdyZWVtZW50LgoKSW5kaWFuYSBVbml2ZXJzaXR5IHdpbGwgY2xlYXJseSBpZGVudGlmeSB5b3VyIG5hbWUgYXMgdGhlIGNyZWF0b3IgYW5kL29yIGNvcHlyaWdodCBvd25lciBvZiB0aGUgc3VibWlzc2lvbiwgYW5kIHdpbGwgbm90IG1ha2UgYW55IGFsdGVyYXRpb24sIG90aGVyIHRoYW4gYXMgYWxsb3dlZCBieSB0aGlzIGxpY2Vuc2UsIHRvIHlvdXIgc3VibWlzc2lvbi4gV2UgYWdyZWUgdG8gbm90IG1ha2UgYXZhaWxhYmxlIGFueSBmaWxlcyB0aGF0IGFyZSBlbWJhcmdvZWQgdW50aWwgdGhlIGVtYmFyZ28gaGFzIGV4cGlyZWQuCgpJZiB5b3UgYXJlIHN1Ym1pdHRpbmcgdGhpcyBpdGVtIG9uIGJlaGFsZiBvZiB0aGUgcmlnaHRzIGhvbGRlciwgeW91IG11c3QgaGF2ZSB0aGUgcmlnaHRzIG93bmVyJ3Mgd3JpdHRlbiBwZXJtaXNzaW9uIHRvIGFjY2VwdCB0aGlzIGxpY2Vuc2Ugb24gaGlzL2hlciBiZWhhbGYuCgo=
oai:scholarworks.iu.edu:2022/190552021-10-18T12:41:19Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Kafka, S.
Honeycutt, R.K.
Williams, R.
2014-10-23T19:35:39Z
2014-10-23T19:35:39Z
2012
Kafka, S., Honeycutt, R. K., & Williams, R. (2012). QU Carinae: Type Ia supernova in the making? Monthly Notices of the Royal Astronomical Society, 425(2), 1585-1590. http://dx.doi.org/10.1111/j.1365-2966.2012.21618.x
http://hdl.handle.net/2022/19055
Variable Na I absorption lines have been reported in a number of Type Ia supernovae (SNeIa). The presence of this circumstellar material suggests that cataclysmic variables (CVs) with a giant donor star may be the progenitors of these SNeIa. We present echelle spectra of the CV QU Carinae which strengthen the connection between CVs of the V Sge class, the accretion wind evolution scenario, variable wind features, variable Na I absorption and SNeIa. This thread not only provides insight into the spectral peculiarities of QU Car, but also links SNeIa as a class with their parent systems.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-23T19:35:39Z
No. of bitstreams: 1
MNRAS-2012-Kafka-1585-90.pdf: 726606 bytes, checksum: bcbd187f47fce083ddb927319b78c6bc (MD5)
Made available in DSpace on 2014-10-23T19:35:39Z (GMT). No. of bitstreams: 1
MNRAS-2012-Kafka-1585-90.pdf: 726606 bytes, checksum: bcbd187f47fce083ddb927319b78c6bc (MD5)
Previous issue date: 2012
en_US
Oxford University Press on behalf of the Royal Astronomical Society
https://doi.org/10.1111/j.1365-2966.2012.21618.x
© 2012 The Authors
novae
cataclysmic variables
supernova: general
QU Carinae: Type Ia supernova in the making?
Article
true
ORIGINAL
MNRAS-2012-Kafka-1585-90.pdf
MNRAS-2012-Kafka-1585-90.pdf
application/pdf
726606
https://scholarworks.iu.edu/dspace/bitstream/2022/19055/1/MNRAS-2012-Kafka-1585-90.pdf
bcbd187f47fce083ddb927319b78c6bc
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19055/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
honeycutt_kent_license_2012.txt
honeycutt_kent_license_2012.txt
text/plain
5189
https://scholarworks.iu.edu/dspace/bitstream/2022/19055/3/honeycutt_kent_license_2012.txt
785857978a55fc8c796b44bb20c5dd3a
MD5
3
TEXT
MNRAS-2012-Kafka-1585-90.pdf.txt
MNRAS-2012-Kafka-1585-90.pdf.txt
Extracted text
text/plain
33826
https://scholarworks.iu.edu/dspace/bitstream/2022/19055/4/MNRAS-2012-Kafka-1585-90.pdf.txt
30e3ed8c109068464545393e12bc60e8
MD5
4
THUMBNAIL
MNRAS-2012-Kafka-1585-90.pdf.jpg
MNRAS-2012-Kafka-1585-90.pdf.jpg
IM Thumbnail
image/jpeg
3577
https://scholarworks.iu.edu/dspace/bitstream/2022/19055/5/MNRAS-2012-Kafka-1585-90.pdf.jpg
2c33ff62b77cd00bf2cfe42abeca0ded
MD5
5
2022/19055
oai:scholarworks.iu.edu:2022/19055
2021-10-18 08:41:19.362
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190662021-10-18T13:48:43Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Michael, S.
Steiman-Cameron, T.Y.
Durisen, R.H.
Boley, A.C.
2014-10-27T17:12:07Z
2014-10-27T17:12:07Z
2012
Michael, S., Steiman-Cameron, T. Y., Durisen, R. H., & Boley, A. C. (2012). Convergence studies of mass transport in disks with gravitational instabilities. I. the constant cooling time case. Astrophysical Journal, 746(1). http://dx.doi.org/10.1088/0004-637X/746/1/98
http://hdl.handle.net/2022/19066
We conduct a convergence study of a protostellar disk, subject to a constant global cooling time and susceptible to gravitational instabilities (GIs), at a time when heating and cooling are roughly balanced. Our goal is to determine the gravitational torques produced by GIs, the level to which transport can be represented by a simple α-disk formulation, and to examine fragmentation criteria. Four simulations are conducted, identical except for the number of azimuthal computational grid points used. A Fourier decomposition of non-axisymmetric density structures in cos ($m\phi$), sin ($m\phi$) is performed to evaluate the amplitudes $A_{m}$ of these structures. The $A_{m}$, gravitational torques, and the effective Shakura & Sunyaev α arising from gravitational stresses are determined for each resolution. We find nonzero $A_{m}$ for all $m$-values and that $A_{m}$ summed over all $m$ is essentially independent of resolution. Because the number of measurable $m$-values is limited to half the number of azimuthal grid points, higher-resolution simulations have a larger fraction of their total amplitude in higher-order structures. These structures act more locally than lower-order structures. Therefore, as the resolution increases the total gravitational stress decreases as well, leading higher-resolution simulations to experience weaker average gravitational torques than lower-resolution simulations. The effective $\alpha$ also depends upon the magnitude of the stresses, thus $\alpha_{\text{eff}}$ also decreases with increasing resolution. Our converged $\alpha_{\text{eff}}$ is consistent with predictions from an analytic local theory for thin disks by Gammie, but only over many dynamic times when averaged over a substantial volume of the disk.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-27T17:12:07Z
No. of bitstreams: 1
0004-637X_746_1_98.pdf: 918617 bytes, checksum: 78e7c8d2b2f858ca7e0f389fd289582e (MD5)
Made available in DSpace on 2014-10-27T17:12:07Z (GMT). No. of bitstreams: 1
0004-637X_746_1_98.pdf: 918617 bytes, checksum: 78e7c8d2b2f858ca7e0f389fd289582e (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/746/1/98
© 2012 The American Astronomical Society. All rights reserved.
accretion
accretion disks
protoplanetary disks
stars: formation
Convergence studies of mass transport in disks with gravitational instabilities. I. the constant cooling time case
Article
false
ORIGINAL
0004-637X_746_1_98.pdf
0004-637X_746_1_98.pdf
application/pdf
918617
https://scholarworks.iu.edu/dspace/bitstream/2022/19066/1/0004-637X_746_1_98.pdf
78e7c8d2b2f858ca7e0f389fd289582e
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19066/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
michael_scott_license_2012.txt
michael_scott_license_2012.txt
text/plain
5938
https://scholarworks.iu.edu/dspace/bitstream/2022/19066/3/michael_scott_license_2012.txt
095ff3ffd486f914dfaf182c256bedb2
MD5
3
TEXT
0004-637X_746_1_98.pdf.txt
0004-637X_746_1_98.pdf.txt
Extracted text
text/plain
60803
https://scholarworks.iu.edu/dspace/bitstream/2022/19066/4/0004-637X_746_1_98.pdf.txt
b5af7d7b51ec03d5ee16283cc0b9bae8
MD5
4
THUMBNAIL
0004-637X_746_1_98.pdf.jpg
0004-637X_746_1_98.pdf.jpg
IM Thumbnail
image/jpeg
2462
https://scholarworks.iu.edu/dspace/bitstream/2022/19066/5/0004-637X_746_1_98.pdf.jpg
fb18d9e4484c2c75c56f46708d5341bf
MD5
5
2022/19066
oai:scholarworks.iu.edu:2022/19066
2021-10-18 09:48:43.699
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190682021-10-18T14:04:15Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Geisler, D.
Villanova, S.
Carraro, G.
Pilachowski, C.A.
Cummings, J.
Johnson, C.I.
Bresolin, F.
2014-10-27T19:30:56Z
2014-10-27T19:30:56Z
2012
Geisler, D., Villanova, S., Carraro, G., Pilachowski, C., Cummings, J., Johnson, C. I., & Bresolin, F. (2012). The unique Na:O abundance distribution in NGC6791: The first open(?) cluster with multiple populations. Astrophysical Journal Letters, 756(2), L40. http://dx.doi.org/10.1088/2041-8205/756/2/L40
http://hdl.handle.net/2022/19068
Almost all globular clusters investigated exhibit a spread in their light element abundances, the most studied being an Na:O anticorrelation. In contrast, open clusters show a homogeneous composition and are still regarded as Simple Stellar Populations. The most probable reason for this difference is that globulars had an initial mass high enough to retain primordial gas and ejecta from the first stellar generation and thus formed a second generation with a distinct composition, an initial mass exceeding that of open clusters. NGC 6791 is a massive open cluster and warrants a detailed search for chemical inhomogeneities. We collected high-resolution, high signal-to-noise spectra of 21 members covering a wide range of evolutionary status and measured their Na, O, and Fe content. We found [Fe/H] = +0.42 ± 0.01, in good agreement with previous values, and no evidence for a spread. However, the Na:O distribution is completely unprecedented. It becomes the first open cluster to show intrinsic abundance variations that cannot be explained by mixing, and thus the first discovered to host multiple populations. It is also the first star cluster to exhibit two subpopulations in the Na:O diagram with one being chemically homogeneous while the second has an intrinsic spread that follows the anticorrelation so far displayed only by globular clusters. NGC 6791 is unique in many aspects, displaying certain characteristics typical of open clusters, others more reminiscent of globulars, and yet others, in particular its Na:O behavior investigated here, that are totally unprecedented. It clearly had a complex and fascinating history.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-27T19:30:56Z
No. of bitstreams: 1
2041-8205_756_2_L40.pdf: 411059 bytes, checksum: 44d32930bc81911124052ed93566b363 (MD5)
Made available in DSpace on 2014-10-27T19:30:56Z (GMT). No. of bitstreams: 1
2041-8205_756_2_L40.pdf: 411059 bytes, checksum: 44d32930bc81911124052ed93566b363 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/2041-8205/756/2/L40
© 2012 The American Astronomical Society
open clusters and associations: individual (NGC 6791)
stars: abundances
The unique Na:O abundance distribution in NGC6791: The first open(?) cluster with multiple populations
Article
true
ORIGINAL
2041-8205_756_2_L40.pdf
2041-8205_756_2_L40.pdf
application/pdf
411059
https://scholarworks.iu.edu/dspace/bitstream/2022/19068/1/2041-8205_756_2_L40.pdf
44d32930bc81911124052ed93566b363
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19068/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
pilachowski_caty_license_2012.txt
pilachowski_caty_license_2012.txt
text/plain
4911
https://scholarworks.iu.edu/dspace/bitstream/2022/19068/3/pilachowski_caty_license_2012.txt
3574483ec4970f72b01f4583eda3b7e3
MD5
3
TEXT
2041-8205_756_2_L40.pdf.txt
2041-8205_756_2_L40.pdf.txt
Extracted text
text/plain
29652
https://scholarworks.iu.edu/dspace/bitstream/2022/19068/4/2041-8205_756_2_L40.pdf.txt
86933d11267e1578e8ca08a6b4f38fb7
MD5
4
THUMBNAIL
2041-8205_756_2_L40.pdf.jpg
2041-8205_756_2_L40.pdf.jpg
IM Thumbnail
image/jpeg
2337
https://scholarworks.iu.edu/dspace/bitstream/2022/19068/5/2041-8205_756_2_L40.pdf.jpg
8778b10a8bbc0eca6d4d1ed5d6a6f162
MD5
5
2022/19068
oai:scholarworks.iu.edu:2022/19068
2021-10-18 10:04:15.427
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190692021-10-18T14:04:11Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Johnson, C.I.
Pilachowski, C.A.
2014-10-27T19:36:30Z
2014-10-27T19:36:30Z
2012
Johnson, C. I., & Pilachowski, C. A. (2012). Oxygen and sodium abundances in M13 (NGC6205) giants: Linking globular cluster formation scenarios, deep mixing, and post-RGB evolution. Astrophysical Journal Letters, 754(2), L38. http://dx.doi.org/10.1088/2041-8205/754/2/L38
http://hdl.handle.net/2022/19069
We present O, Na, and Fe abundances, as well as radial velocities, for 113 red giant branch (RGB) and asymptotic giant branch (AGB) stars in the globular cluster M13. The abundances and velocities are based on spectra obtained with the WIYN-Hydra spectrograph, and the observations range in luminosity from the horizontal branch (HB) to RGB tip. The results are examined in the context of recent globular cluster formation scenarios. We find that M13 exhibits many key characteristics that suggest its formation and chemical enrichment are well described by current models. Some of these observations include the central concentration of O-poor stars, the notable decrease in [O/Fe] (but small increase in [Na/Fe]) with increasing luminosity that affects primarily the "extreme" population, the small fraction of stars with halo-like composition, and the paucity of O-poor AGB stars. In agreement with recent work, we conclude that the most O-poor M13 giants are likely He-enriched and that most (all?) O-poor RGB stars evolve to become extreme HB and AGB-manqué stars. In contrast, the "primordial" and "intermediate" population stars appear to experience standard HB and AGB evolution.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-27T19:36:30Z
No. of bitstreams: 1
2041-8205_754_2_L38.pdf: 538466 bytes, checksum: b4727092a23c5574c814e8f99eab5f57 (MD5)
Made available in DSpace on 2014-10-27T19:36:30Z (GMT). No. of bitstreams: 1
2041-8205_754_2_L38.pdf: 538466 bytes, checksum: b4727092a23c5574c814e8f99eab5f57 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/2041-8205/754/2/L38
© 2012 The American Astronomical Society
Galaxy: halo
globular clusters: genera
globular clusters: individual (M13, NGC 6205)
stars: abundances
stars: Population II
Oxygen and sodium abundances in M13 (NGC6205) giants: Linking globular cluster formation scenarios, deep mixing, and post-RGB evolution
Article
false
ORIGINAL
2041-8205_754_2_L38.pdf
2041-8205_754_2_L38.pdf
application/pdf
538466
https://scholarworks.iu.edu/dspace/bitstream/2022/19069/1/2041-8205_754_2_L38.pdf
b4727092a23c5574c814e8f99eab5f57
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19069/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
pilachowski_caty_license_2012.txt
pilachowski_caty_license_2012.txt
text/plain
4911
https://scholarworks.iu.edu/dspace/bitstream/2022/19069/3/pilachowski_caty_license_2012.txt
3574483ec4970f72b01f4583eda3b7e3
MD5
3
TEXT
2041-8205_754_2_L38.pdf.txt
2041-8205_754_2_L38.pdf.txt
Extracted text
text/plain
30106
https://scholarworks.iu.edu/dspace/bitstream/2022/19069/4/2041-8205_754_2_L38.pdf.txt
6e937fa9a7bc869dbbdc5cc7fc38b3d6
MD5
4
THUMBNAIL
2041-8205_754_2_L38.pdf.jpg
2041-8205_754_2_L38.pdf.jpg
IM Thumbnail
image/jpeg
2341
https://scholarworks.iu.edu/dspace/bitstream/2022/19069/5/2041-8205_754_2_L38.pdf.jpg
cf155c5ce7af77ed3b90460114f335fe
MD5
5
2022/19069
oai:scholarworks.iu.edu:2022/19069
2021-10-18 10:04:11.555
IUScholarWorks
iusw@indiana.edu
CkJ5IHNpZ25pbmcgYW5kIHN1Ym1pdHRpbmcgdGhpcyBsaWNlbnNlLCB5b3UgKHRoZSBjcmVhdG9yIG9yIGNvcHlyaWdodCBvd25lcikgZ3JhbnQgdG8gSW5kaWFuYSBVbml2ZXJzaXR5IGEgbm9uLWV4Y2x1c2l2ZSwgcGVycGV0dWFsLCBpcnJldm9jYWJsZSByaWdodCB0byByZXByb2R1Y2UsIHRyYW5zbGF0ZSAoYXMgZGVmaW5lZCBiZWxvdyksIGFuZC9vciBkaXN0cmlidXRlIHlvdXIgc3VibWlzc2lvbiAoaW5jbHVkaW5nIHRoZSBhYnN0cmFjdCkgd29ybGR3aWRlIGluIHByaW50IGFuZCBlbGVjdHJvbmljIGZvcm1hdCBhbmQgaW4gYW55IG1lZGl1bSwgaW5jbHVkaW5nIGJ1dCBub3QgbGltaXRlZCB0byBhdWRpbyBvciB2aWRlby4KCllvdSBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXksIHdpdGhvdXQgY2hhbmdpbmcgdGhlIGNvbnRlbnQsIHRyYW5zbGF0ZSB0aGUgc3VibWlzc2lvbiB0byBhbnkgbWVkaXVtIG9yIGZvcm1hdCBmb3IgcHJlc2VydmF0aW9uIG9yIGFjY2VzcywgYW5kIHByb3ZpZGUgYmFzaWMgbWV0YWRhdGEgdGhhdCBkZXNjcmliZXMgdGhlIGNvbnRlbnRzIGZvciBkaXNjb3ZlcnkuCgpZb3UgYWxzbyBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXkga2VlcCBtb3JlIHRoYW4gb25lIGNvcHkgb2YgdGhpcyBzdWJtaXNzaW9uIGZvciBzZWN1cml0eSwgYmFjay11cCBhbmQgcHJlc2VydmF0aW9uLgoKWW91IHJlcHJlc2VudCB0aGF0IHRoZSBzdWJtaXNzaW9uIGlzIHlvdXIgb3JpZ2luYWwgd29yaywgYW5kIHRoYXQgeW91IGhhdmUgdGhlIHJpZ2h0IHRvIGdyYW50IHRoZSByaWdodHMgY29udGFpbmVkIGluIHRoaXMgbGljZW5zZS4gWW91IGFsc28gcmVwcmVzZW50IHRoYXQgeW91ciBzdWJtaXNzaW9uIGRvZXMgbm90LCB0byB0aGUgYmVzdCBvZiB5b3VyIGtub3dsZWRnZSwgaW5mcmluZ2UgdXBvbiBhbnlvbmUncyBjb3B5cmlnaHQuCgpJZiB0aGUgc3VibWlzc2lvbiBjb250YWlucyBtYXRlcmlhbCBmb3Igd2hpY2ggeW91IGRvIG5vdCBob2xkIGNvcHlyaWdodCwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIG9idGFpbmVkIHRoZSB1bnJlc3RyaWN0ZWQgcGVybWlzc2lvbiBvZiB0aGUgY29weXJpZ2h0IG93bmVyIHRvIGdyYW50IEluZGlhbmEgVW5pdmVyc2l0eSB0aGUgcmlnaHRzIHJlcXVpcmVkIGJ5IHRoaXMgbGljZW5zZSwgYW5kIHRoYXQgc3VjaCB0aGlyZC1wYXJ0eSBvd25lZCBtYXRlcmlhbCBpcyBjbGVhcmx5IGlkZW50aWZpZWQgYW5kIGFja25vd2xlZGdlZCB3aXRoaW4gdGhlIHRleHQgb3IgY29udGVudCBvZiB0aGUgc3VibWlzc2lvbi4KCklmIHRoZSBzdWJtaXNzaW9uIGlzIGJhc2VkIHVwb24gd29yayB0aGF0IGhhcyBiZWVuIHNwb25zb3JlZCBvciBzdXBwb3J0ZWQgYnkgYW4gYWdlbmN5IG9yIG9yZ2FuaXphdGlvbiBvdGhlciB0aGFuIEluZGlhbmEgVW5pdmVyc2l0eSwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIGZ1bGZpbGxlZCBhbnkgcmlnaHQgb2YgcmV2aWV3IG9yIG90aGVyIG9ibGlnYXRpb25zIHJlcXVpcmVkIGJ5IHN1Y2ggY29udHJhY3Qgb3IgYWdyZWVtZW50LgoKSW5kaWFuYSBVbml2ZXJzaXR5IHdpbGwgY2xlYXJseSBpZGVudGlmeSB5b3VyIG5hbWUgYXMgdGhlIGNyZWF0b3IgYW5kL29yIGNvcHlyaWdodCBvd25lciBvZiB0aGUgc3VibWlzc2lvbiwgYW5kIHdpbGwgbm90IG1ha2UgYW55IGFsdGVyYXRpb24sIG90aGVyIHRoYW4gYXMgYWxsb3dlZCBieSB0aGlzIGxpY2Vuc2UsIHRvIHlvdXIgc3VibWlzc2lvbi4gV2UgYWdyZWUgdG8gbm90IG1ha2UgYXZhaWxhYmxlIGFueSBmaWxlcyB0aGF0IGFyZSBlbWJhcmdvZWQgdW50aWwgdGhlIGVtYmFyZ28gaGFzIGV4cGlyZWQuCgpJZiB5b3UgYXJlIHN1Ym1pdHRpbmcgdGhpcyBpdGVtIG9uIGJlaGFsZiBvZiB0aGUgcmlnaHRzIGhvbGRlciwgeW91IG11c3QgaGF2ZSB0aGUgcmlnaHRzIG93bmVyJ3Mgd3JpdHRlbiBwZXJtaXNzaW9uIHRvIGFjY2VwdCB0aGlzIGxpY2Vuc2Ugb24gaGlzL2hlciBiZWhhbGYuCgo=
oai:scholarworks.iu.edu:2022/190772021-10-18T12:41:40Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Hargis, J.R.
Rhode, K.L.
2014-10-30T18:54:55Z
2014-10-30T18:54:55Z
2012
Hargis, J. R., & Rhode, K. L. (2012). The globular cluster populations of giant galaxies: Mosaic imaging of five moderate-luminosity early-type galaxies. Astronomical Journal, 144(6), 164. http://dx.doi.org/10.1088/0004-6256/144/6/164
http://hdl.handle.net/2022/19077
This paper presents results from wide-field imaging of the globular cluster (GC) systems of five intermediate-luminosity ($M_{V}$ ~ –21 to –22) early-type galaxies. The aim is to accurately quantify the global properties of the GC systems by measuring them out to large radii. We obtained BVR imaging of four lenticular galaxies (NGC 5866, NGC 4762, NGC 4754, NGC 3384) and one elliptical galaxy (NGC 5813) using the KPNO 4 m telescope and Mosaic imager and traced the GC population to projected galactocentric radii ranging from ~20 kpc to 120 kpc. We combine our imaging with Hubble Space Telescope data to measure the GC surface density close to the galaxy center. We calculate the total number of GCs (N GC) from the integrated radial profile and find $N_{GC}$ = 340 ± 80 for NGC 5866, $N_{GC}$ = 2900 ± 400 for NGC 5813, $N_{GC}$ = 270 ± 30 for NGC 4762, $N_{GC}$ = 115 ± 15 for NGC 4754, and $N_{GC}$ = 120 ± 30 for NGC 3384. The measured GC specific frequencies are SN between 0.6 and 3.6 and T in the range 0.9-4.2. These values are consistent with the mean specific frequencies for the galaxies' morphological types found by our survey and other published data. Three galaxies (NGC 5866, NGC 5813, and NGC 4762) had sufficient numbers of GC candidates to investigate color bimodality and color gradients in the GC systems. NGC 5813 shows strong evidence (>3σ) for bimodality and a B – R color gradient resulting from a more centrally concentrated red (metal-rich) GC subpopulation. We find no evidence for statistically significant color gradients in the other two galaxies.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T18:54:55Z
No. of bitstreams: 1
1538-3881_144_6_164.pdf: 4077242 bytes, checksum: 5663a7f9fe6d5178d544bb1837c00507 (MD5)
Made available in DSpace on 2014-10-30T18:54:55Z (GMT). No. of bitstreams: 1
1538-3881_144_6_164.pdf: 4077242 bytes, checksum: 5663a7f9fe6d5178d544bb1837c00507 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-6256/144/6/164
© 2012 The American Astronomical Society
galaxies: elliptical and lenticular, cD
galaxies: formation
galaxies: photometry
galaxies: star clusters: general
galaxies: individual (NGC 5866, NGC 5813, NGC 4762, NGC 4754, NGC 3384)
The globular cluster populations of giant galaxies: Mosaic imaging of five moderate-luminosity early-type galaxies
Article
false
ORIGINAL
1538-3881_144_6_164.pdf
1538-3881_144_6_164.pdf
application/pdf
4077242
https://scholarworks.iu.edu/dspace/bitstream/2022/19077/1/1538-3881_144_6_164.pdf
5663a7f9fe6d5178d544bb1837c00507
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19077/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
rhode_katherine_license_2012.txt
rhode_katherine_license_2012.txt
text/plain
5370
https://scholarworks.iu.edu/dspace/bitstream/2022/19077/3/rhode_katherine_license_2012.txt
558f25fcdf616d4576aa18a64baf5a41
MD5
3
TEXT
1538-3881_144_6_164.pdf.txt
1538-3881_144_6_164.pdf.txt
Extracted text
text/plain
100340
https://scholarworks.iu.edu/dspace/bitstream/2022/19077/4/1538-3881_144_6_164.pdf.txt
19ebaefa273c46194e3a4572fe3c3b71
MD5
4
THUMBNAIL
1538-3881_144_6_164.pdf.jpg
1538-3881_144_6_164.pdf.jpg
IM Thumbnail
image/jpeg
2387
https://scholarworks.iu.edu/dspace/bitstream/2022/19077/5/1538-3881_144_6_164.pdf.jpg
2356450118997ee51641e62dec94aa91
MD5
5
2022/19077
oai:scholarworks.iu.edu:2022/19077
2021-10-18 08:41:40.747
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190782021-10-18T13:12:22Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Matheson, T.
Joyce, R.R.
Allen, L.E.
Saha, A.
Silva, D.R.
Wood-Vasey, W.M.
Adams, J.J.
Anderson, R.E.
Beck, T.L.
Bentz, M.C.
Bershady, M.A.
Binkert, W.S.
Butler, K.
Camarata, M.A.
Eigenbrot, A.
Everett, M.
Gallagher, J.S.
Garnavich, P.M.
Glikman, E.
Harbeck, D.
Hargis, J.R.
Herbst, H.
Horch, E.P.
Howell, S.B.
Jha, S.
Kaczmarek, J.F.
Knezek, P.
Manne-Nicholas, E.
Mathieu, R.D.
Meixner, M.
Milliman, K.
Power, J.
Rajagopal, J.
Reetz, K.
Rhode, K.L.
Schechtman-Rook, A.
Schwamb, M.E.
Schweiker, H.
Simmons, B.
Simon, J.D.
Summers, D.
Young, M.D.
Weyant, A.
Wilcots, E.M.
Will, G.
Williams, D.
2014-10-30T19:04:25Z
2014-10-30T19:04:25Z
2012
Matheson, T., Joyce, R. R., Allen, L. E., Saha, A., Silva, D. R., Wood-Vasey, W. M., . . . Williams, D. (2012). The infrared light curve of SN 2011fe in M101 and the distance to M101. Astrophysical Journal, 754(1), 19. http://dx.doi.org/10.1088/0004-637X/754/1/19
http://hdl.handle.net/2022/19078
We present near-infrared light curves of supernova (SN) 2011fe in M101, including 34 epochs in H band starting 14 days before maximum brightness in the B band. The light curve data were obtained with the WIYN High-Resolution Infrared Camera. When the data are calibrated using templates of other Type Ia SNe, we derive an apparent H-band magnitude at the epoch of B-band maximum of 10.85 ± 0.04. This implies a distance modulus for M101 that ranges from 28.86 to 29.17 mag, depending on which absolute calibration for Type Ia SNe is used.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T19:04:25Z
No. of bitstreams: 1
0004-637X_754_1_19.pdf: 314760 bytes, checksum: a562bc9ce2a112843779a0e844121774 (MD5)
Made available in DSpace on 2014-10-30T19:04:25Z (GMT). No. of bitstreams: 1
0004-637X_754_1_19.pdf: 314760 bytes, checksum: a562bc9ce2a112843779a0e844121774 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/754/1/19
© 2012 The American Astronomical Society.
galaxies: distances and redshifts
galaxies: individual (M101)
supernovae: individual (SN 2011fe)
The infrared light curve of SN 2011fe in M101 and the distance to M101
Article
false
ORIGINAL
0004-637X_754_1_19.pdf
0004-637X_754_1_19.pdf
application/pdf
314760
https://scholarworks.iu.edu/dspace/bitstream/2022/19078/1/0004-637X_754_1_19.pdf
a562bc9ce2a112843779a0e844121774
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19078/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
rhode_katherine_license_2012.txt
rhode_katherine_license_2012.txt
text/plain
5370
https://scholarworks.iu.edu/dspace/bitstream/2022/19078/3/rhode_katherine_license_2012.txt
558f25fcdf616d4576aa18a64baf5a41
MD5
3
TEXT
0004-637X_754_1_19.pdf.txt
0004-637X_754_1_19.pdf.txt
Extracted text
text/plain
32085
https://scholarworks.iu.edu/dspace/bitstream/2022/19078/4/0004-637X_754_1_19.pdf.txt
15a83ad02f91f05acf613f4c1aca871f
MD5
4
THUMBNAIL
0004-637X_754_1_19.pdf.jpg
0004-637X_754_1_19.pdf.jpg
IM Thumbnail
image/jpeg
2375
https://scholarworks.iu.edu/dspace/bitstream/2022/19078/5/0004-637X_754_1_19.pdf.jpg
eb5f7affb1bcd64e6871f7efadac57b4
MD5
5
2022/19078
oai:scholarworks.iu.edu:2022/19078
2021-10-18 09:12:22.941
IUScholarWorks
iusw@indiana.edu
CkJ5IHNpZ25pbmcgYW5kIHN1Ym1pdHRpbmcgdGhpcyBsaWNlbnNlLCB5b3UgKHRoZSBjcmVhdG9yIG9yIGNvcHlyaWdodCBvd25lcikgZ3JhbnQgdG8gSW5kaWFuYSBVbml2ZXJzaXR5IGEgbm9uLWV4Y2x1c2l2ZSwgcGVycGV0dWFsLCBpcnJldm9jYWJsZSByaWdodCB0byByZXByb2R1Y2UsIHRyYW5zbGF0ZSAoYXMgZGVmaW5lZCBiZWxvdyksIGFuZC9vciBkaXN0cmlidXRlIHlvdXIgc3VibWlzc2lvbiAoaW5jbHVkaW5nIHRoZSBhYnN0cmFjdCkgd29ybGR3aWRlIGluIHByaW50IGFuZCBlbGVjdHJvbmljIGZvcm1hdCBhbmQgaW4gYW55IG1lZGl1bSwgaW5jbHVkaW5nIGJ1dCBub3QgbGltaXRlZCB0byBhdWRpbyBvciB2aWRlby4KCllvdSBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXksIHdpdGhvdXQgY2hhbmdpbmcgdGhlIGNvbnRlbnQsIHRyYW5zbGF0ZSB0aGUgc3VibWlzc2lvbiB0byBhbnkgbWVkaXVtIG9yIGZvcm1hdCBmb3IgcHJlc2VydmF0aW9uIG9yIGFjY2VzcywgYW5kIHByb3ZpZGUgYmFzaWMgbWV0YWRhdGEgdGhhdCBkZXNjcmliZXMgdGhlIGNvbnRlbnRzIGZvciBkaXNjb3ZlcnkuCgpZb3UgYWxzbyBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXkga2VlcCBtb3JlIHRoYW4gb25lIGNvcHkgb2YgdGhpcyBzdWJtaXNzaW9uIGZvciBzZWN1cml0eSwgYmFjay11cCBhbmQgcHJlc2VydmF0aW9uLgoKWW91IHJlcHJlc2VudCB0aGF0IHRoZSBzdWJtaXNzaW9uIGlzIHlvdXIgb3JpZ2luYWwgd29yaywgYW5kIHRoYXQgeW91IGhhdmUgdGhlIHJpZ2h0IHRvIGdyYW50IHRoZSByaWdodHMgY29udGFpbmVkIGluIHRoaXMgbGljZW5zZS4gWW91IGFsc28gcmVwcmVzZW50IHRoYXQgeW91ciBzdWJtaXNzaW9uIGRvZXMgbm90LCB0byB0aGUgYmVzdCBvZiB5b3VyIGtub3dsZWRnZSwgaW5mcmluZ2UgdXBvbiBhbnlvbmUncyBjb3B5cmlnaHQuCgpJZiB0aGUgc3VibWlzc2lvbiBjb250YWlucyBtYXRlcmlhbCBmb3Igd2hpY2ggeW91IGRvIG5vdCBob2xkIGNvcHlyaWdodCwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIG9idGFpbmVkIHRoZSB1bnJlc3RyaWN0ZWQgcGVybWlzc2lvbiBvZiB0aGUgY29weXJpZ2h0IG93bmVyIHRvIGdyYW50IEluZGlhbmEgVW5pdmVyc2l0eSB0aGUgcmlnaHRzIHJlcXVpcmVkIGJ5IHRoaXMgbGljZW5zZSwgYW5kIHRoYXQgc3VjaCB0aGlyZC1wYXJ0eSBvd25lZCBtYXRlcmlhbCBpcyBjbGVhcmx5IGlkZW50aWZpZWQgYW5kIGFja25vd2xlZGdlZCB3aXRoaW4gdGhlIHRleHQgb3IgY29udGVudCBvZiB0aGUgc3VibWlzc2lvbi4KCklmIHRoZSBzdWJtaXNzaW9uIGlzIGJhc2VkIHVwb24gd29yayB0aGF0IGhhcyBiZWVuIHNwb25zb3JlZCBvciBzdXBwb3J0ZWQgYnkgYW4gYWdlbmN5IG9yIG9yZ2FuaXphdGlvbiBvdGhlciB0aGFuIEluZGlhbmEgVW5pdmVyc2l0eSwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIGZ1bGZpbGxlZCBhbnkgcmlnaHQgb2YgcmV2aWV3IG9yIG90aGVyIG9ibGlnYXRpb25zIHJlcXVpcmVkIGJ5IHN1Y2ggY29udHJhY3Qgb3IgYWdyZWVtZW50LgoKSW5kaWFuYSBVbml2ZXJzaXR5IHdpbGwgY2xlYXJseSBpZGVudGlmeSB5b3VyIG5hbWUgYXMgdGhlIGNyZWF0b3IgYW5kL29yIGNvcHlyaWdodCBvd25lciBvZiB0aGUgc3VibWlzc2lvbiwgYW5kIHdpbGwgbm90IG1ha2UgYW55IGFsdGVyYXRpb24sIG90aGVyIHRoYW4gYXMgYWxsb3dlZCBieSB0aGlzIGxpY2Vuc2UsIHRvIHlvdXIgc3VibWlzc2lvbi4gV2UgYWdyZWUgdG8gbm90IG1ha2UgYXZhaWxhYmxlIGFueSBmaWxlcyB0aGF0IGFyZSBlbWJhcmdvZWQgdW50aWwgdGhlIGVtYmFyZ28gaGFzIGV4cGlyZWQuCgpJZiB5b3UgYXJlIHN1Ym1pdHRpbmcgdGhpcyBpdGVtIG9uIGJlaGFsZiBvZiB0aGUgcmlnaHRzIGhvbGRlciwgeW91IG11c3QgaGF2ZSB0aGUgcmlnaHRzIG93bmVyJ3Mgd3JpdHRlbiBwZXJtaXNzaW9uIHRvIGFjY2VwdCB0aGlzIGxpY2Vuc2Ugb24gaGlzL2hlciBiZWhhbGYuCgo=
oai:scholarworks.iu.edu:2022/190822021-10-18T14:04:33Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Peacock, M.B.
Zepf, S.E.
Kundu, A.
MacCarone, T.J.
Rhode, K.L.
Salzer, J.J.
Waters, C.Z.
Ciardullo, R.
Gronwall, C.
Stern, D.
2014-10-30T19:34:32Z
2014-10-30T19:34:32Z
2012
Peacock, M. B., Zepf, S. E., Kundu, A., MacCarone, T. J., Rhode, K. L., Salzer, J. J., . . . Stern, D. (2012). Spatially resolved spectroscopy of the globular cluster RZ 2109 and the nature of its black hole. Astrophysical Journal, 759(2). http://dx.doi.org/10.1088/0004-637X/759/2/126
http://hdl.handle.net/2022/19082
*Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.
We present optical Hubble Space Telescope/Space Telescope Imaging Spectrograph ($HST/S\text{TIS}$) spectroscopy of RZ 2109, a globular cluster (GC) in the elliptical galaxy NGC 4472. This GC is notable for hosting an ultraluminous X-ray source as well as associated strong and broad [O III] $\lambda\lambda4959$, 5007 emission. We show that the $HST/S\text{TIS}$ spectroscopy spatially resolves the [O III] emission in RZ 2109. While we are unable to make a precise determination of the morphology of the emission-line nebula, the best-fitting models all require that the [O III] $\lambda5007$ emission has a half-light radius in the range 3-7 pc. The extended nature of the [O III] $\lambda5007$ emission is inconsistent with published models that invoke an intermediate-mass black hole origin. It is also inconsistent with the ionization of ejecta from a nova in the cluster. The spatial scale of the nebula could be produced via the photoionization of a strong wind driven from a stellar mass black hole accreting at roughly its Eddington rate.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T19:34:32Z
No. of bitstreams: 1
0004-637X_759_2_126.pdf: 323488 bytes, checksum: 5c26d42d275651fd4210f36af489b920 (MD5)
Made available in DSpace on 2014-10-30T19:34:32Z (GMT). No. of bitstreams: 1
0004-637X_759_2_126.pdf: 323488 bytes, checksum: 5c26d42d275651fd4210f36af489b920 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/759/2/126
© 2012 The American Astronomical Society
galaxies: individual (NGC 4472)
galaxies: star clusters: general
galaxies: star clusters: individual (RZ 2109)
globular clusters: general
X-rays: binaries
X-rays: galaxies: clusters
Spatially resolved spectroscopy of the globular cluster RZ 2109 and the nature of its black hole*
Article
false
ORIGINAL
0004-637X_759_2_126.pdf
0004-637X_759_2_126.pdf
application/pdf
323488
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/1/0004-637X_759_2_126.pdf
5c26d42d275651fd4210f36af489b920
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
rhode_katherine_license_2012.txt
rhode_katherine_license_2012.txt
text/plain
5370
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/3/rhode_katherine_license_2012.txt
558f25fcdf616d4576aa18a64baf5a41
MD5
3
salzer_john_license_2012.txt
salzer_john_license_2012.txt
text/plain
4581
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/4/salzer_john_license_2012.txt
9b1d8f3a4f663a2c76c814bc29c27006
MD5
4
TEXT
0004-637X_759_2_126.pdf.txt
0004-637X_759_2_126.pdf.txt
Extracted text
text/plain
37761
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/5/0004-637X_759_2_126.pdf.txt
68859bbb0b8d46bc2319e5d44aeda8ac
MD5
5
THUMBNAIL
0004-637X_759_2_126.pdf.jpg
0004-637X_759_2_126.pdf.jpg
IM Thumbnail
image/jpeg
2348
https://scholarworks.iu.edu/dspace/bitstream/2022/19082/6/0004-637X_759_2_126.pdf.jpg
78d77ee42a36dd30c08ea9855b8437ea
MD5
6
2022/19082
oai:scholarworks.iu.edu:2022/19082
2021-10-18 10:04:33.382
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190832021-10-18T13:36:34Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Rhode, K.L.
2014-10-30T19:40:53Z
2014-10-30T19:40:53Z
2012
Rhode, K. L. (2012). Exploring the correlations between globular cluster populations and supermassive black holes in giant galaxies. Astronomical Journal, 144(5). http://dx.doi.org/10.1088/0004-6256/144/5/154
http://hdl.handle.net/2022/19083
This paper presents an analysis of the correlation between the number of globular clusters ($N_{GC}$) in giant galaxies and the mass of the galaxies' central supermassive black hole ( $M_{SMBH}$). I construct a sample of 20 elliptical, spiral, and S0 galaxies with known SMBH masses and with accurately measured GC system properties derived from wide-field imaging studies. The coefficients of the best-fitting $N_{GC}-M_{SMBH}$ relation for the early-type galaxies are consistent with those from previous work but in some cases have smaller relative errors. I examine the correlation between $N_{GC}$ and $M_{SMBH}$ for various subsamples and find that elliptical galaxies show the strongest correlation, while S0 and pseudobulge galaxies exhibit increased scatter. I also compare the quality of the fit of the numbers of metal-poor GCs versus SMBH mass and the corresponding fit for metal-rich GCs. I supplement the 20 galaxy sample with 10 additional galaxies with reliable $N_{GC}$ determinations but without measured $M_{SMBH}$. I use this larger sample to investigate correlations between $N_{GC}$ and host galaxy properties like total galaxy luminosity and stellar mass, and bulge luminosity and mass. I find that the tightest correlation is between $N_{GC}$ and total galaxy stellar mass. This lends support to the notion that $N_{GC}$ and $M_{SMBH}$ are not directly linked but are correlated because both quantities depend on the host galaxy potential. Finally, I use the $N_{GC}-M_{SMBH}$ relation derived from the 20 galaxy sample to calculate predicted $M_{SMBH}$ values for the 10 galaxies with accurate $N_{GC}$ measurements but without measured SMBH masses.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T19:40:53Z
No. of bitstreams: 1
1538-3881_144_5_154.pdf: 676075 bytes, checksum: 07c92d58e84d52b9a4c7063a3f34e2e4 (MD5)
Made available in DSpace on 2014-10-30T19:40:53Z (GMT). No. of bitstreams: 1
1538-3881_144_5_154.pdf: 676075 bytes, checksum: 07c92d58e84d52b9a4c7063a3f34e2e4 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-6256/144/5/154
© 2012 The American Astronomical Society
black hole physics
galaxies: elliptical and lenticular, cD
galaxies: formation
galaxies: spiral
galaxies: star clusters: general
globular clusters: general
Exploring the correlations between globular cluster populations and supermassive black holes in giant galaxies
Article
true
ORIGINAL
1538-3881_144_5_154.pdf
1538-3881_144_5_154.pdf
application/pdf
676075
https://scholarworks.iu.edu/dspace/bitstream/2022/19083/1/1538-3881_144_5_154.pdf
07c92d58e84d52b9a4c7063a3f34e2e4
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19083/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
rhode_katherine_license_2012.txt
rhode_katherine_license_2012.txt
text/plain
5370
https://scholarworks.iu.edu/dspace/bitstream/2022/19083/3/rhode_katherine_license_2012.txt
558f25fcdf616d4576aa18a64baf5a41
MD5
3
TEXT
1538-3881_144_5_154.pdf.txt
1538-3881_144_5_154.pdf.txt
Extracted text
text/plain
118550
https://scholarworks.iu.edu/dspace/bitstream/2022/19083/4/1538-3881_144_5_154.pdf.txt
359147de783f8f1eea81641dd2bc37f4
MD5
4
THUMBNAIL
1538-3881_144_5_154.pdf.jpg
1538-3881_144_5_154.pdf.jpg
IM Thumbnail
image/jpeg
2383
https://scholarworks.iu.edu/dspace/bitstream/2022/19083/5/1538-3881_144_5_154.pdf.jpg
3cab76dd8ca8a3fe554612c77113a396
MD5
5
2022/19083
oai:scholarworks.iu.edu:2022/19083
2021-10-18 09:36:34.317
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190842021-10-18T14:15:39Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Richards, E.E.
Lang, C.C.
Trombley, C.
Figer, D.F.
2014-10-30T19:46:42Z
2014-10-30T19:46:42Z
2012
Richards, E. E., Lang, C. C., Trombley, C., & Figer, D. F. (2012). Multiwavelength observations of massive stellar cluster candidates in the galaxy. Astronomical Journal, 144(3), 89. http://dx.doi.org/ 10.1088/0004-6256/144/3/89
http://hdl.handle.net/2022/19084
The Galaxy appears to be richer in young, massive stellar clusters than previously known, due to advances in infrared surveys that have uncovered deeply embedded regions of star formation. Young, massive clusters can significantly impact the surrounding interstellar medium (ISM) and hence radio observations can also be an important tracer of their activity. Several hundred cluster candidates are now known by examining survey data. Here, we report on multiwavelength observations of six of these candidates in the Galaxy. We carried out 4.9 and 8.5 GHz Very Large Array observations of the radio emission associated with these clusters to obtain the physical characteristics of the surrounding gas, including the Lyman continuum photon flux and ionized gas mass. $\textit{Spitzer}$ Infrared Array Camera observations were also made of these regions, and provide details on the stellar population as well as the dust continuum and polycyclic aromatic hydrocarbon emission. When compared to the known young, massive clusters in the Galaxy, the six cluster candidates have less powerful Lyman ionizing fluxes and ionize less of the H II mass in the surrounding ISM. Therefore, these cluster candidates appear to be more consistent with intermediate-mass clusters ($10^{3}-10^{4} M_{\odot}$)
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T19:46:42Z
No. of bitstreams: 1
1538-3881_144_3_89.pdf: 6773599 bytes, checksum: 41a09ca76076e35ad10468d38ceda5c5 (MD5)
Made available in DSpace on 2014-10-30T19:46:42Z (GMT). No. of bitstreams: 1
1538-3881_144_3_89.pdf: 6773599 bytes, checksum: 41a09ca76076e35ad10468d38ceda5c5 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/ 10.1088/0004-6256/144/3/89
© 2012 The American Astronomical Society
evolution
Hii regions
local interstellar matter
stars: massive
Multiwavelength observations of massive stellar cluster candidates in the galaxy
Article
false
ORIGINAL
1538-3881_144_3_89.pdf
1538-3881_144_3_89.pdf
application/pdf
6773599
https://scholarworks.iu.edu/dspace/bitstream/2022/19084/1/1538-3881_144_3_89.pdf
41a09ca76076e35ad10468d38ceda5c5
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19084/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
richards_emily_license_2012.txt
richards_emily_license_2012.txt
text/plain
4370
https://scholarworks.iu.edu/dspace/bitstream/2022/19084/3/richards_emily_license_2012.txt
b1013b8c65e00cb8cfb9ca69c604b191
MD5
3
TEXT
1538-3881_144_3_89.pdf.txt
1538-3881_144_3_89.pdf.txt
Extracted text
text/plain
64697
https://scholarworks.iu.edu/dspace/bitstream/2022/19084/4/1538-3881_144_3_89.pdf.txt
2c228562f383f6e7415340f3389b5c63
MD5
4
THUMBNAIL
1538-3881_144_3_89.pdf.jpg
1538-3881_144_3_89.pdf.jpg
IM Thumbnail
image/jpeg
2396
https://scholarworks.iu.edu/dspace/bitstream/2022/19084/5/1538-3881_144_3_89.pdf.jpg
f7d593877e6675a909a51da5514caf06
MD5
5
2022/19084
oai:scholarworks.iu.edu:2022/19084
2021-10-18 10:15:39.775
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190852021-10-18T13:39:36Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Mostek, N.
Coil, A.L.
Moustakas, J.
Salim, S.
Weiner, B.J.
2014-10-30T19:55:16Z
2014-10-30T19:55:16Z
2012
Mostek, N., Coil, A. L., Moustakas, J., Salim, S., & Weiner, B. J. (2012). Calibrating the star formation rate at $z \sim 1$ from optical data. Astrophysical Journal, 746(2), 124. http://dx.doi.org/10.1088/0004-637X/746/2/124
http://hdl.handle.net/2022/19085
We present a star formation rate (SFR) calibration based on optical data that is consistent with average observed rates in both the red and blue galaxy populations at $z \sim 1$. The motivation for this study is to calculate SFRs for DEEP2 Redshift Survey galaxies in the $0.7 < z < 1.4$ redshift range, but our results are generally applicable to similar optically selected galaxy samples without requiring UV or IR data. Using SFR fits from UV/optical spectral energy distributions (SEDs) in the All-Wavelength Extended Groth Strip International Survey, we explore the behavior of rest-frame B-band magnitude, observed [O II] luminosity, and rest-frame color with SED-fit SFR for both red sequence and blue cloud galaxies. The resulting SFR calibration is based on three optical-band observables: $M_{B} , \big(U – B\big)$, and $\big(B – V\big)$. The best-fit linear relation produces residual errors of 0.3 dex rms scatter for the full color-independent sample with minimal correlated residual error in $L\big[O_{II}\big]$ or stellar mass. We then compare the calibrated $z \sim 1$ SFRs to two diagnostics that use $L\big[O_{II}\big]$ as a tracer in local galaxies and correct for dust extinction at intermediate redshifts through either galaxy $B$-band luminosity or stellar mass. We find that an$ L\big[O_{II}\big]-M_{B}$ SFR calibration commonly used in the literature agrees well with our calculated SFRs after correcting for the average B-band luminosity evolution in $L_{*}$ galaxies. However, we find better agreement with a local $L\big[O_{II}\big]$-based SFR calibration that includes stellar mass to correct for reddening effects, indicating that stellar mass is a better tracer of dust extinction for all galaxy types and less affected by systematic evolution than galaxy luminosity from $z = 1$ to the current epoch.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T19:55:16Z
No. of bitstreams: 1
0004-637X_746_2_124.pdf: 19049609 bytes, checksum: cf88aa642f1e8ca758b9f54dc0878ff2 (MD5)
Made available in DSpace on 2014-10-30T19:55:16Z (GMT). No. of bitstreams: 1
0004-637X_746_2_124.pdf: 19049609 bytes, checksum: cf88aa642f1e8ca758b9f54dc0878ff2 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/746/2/124
© 2012 The American Astronomical Society
galaxies: active
galaxies: evolution
galaxies: high-redshift
Calibrating the star formation rate at $z \sim 1$ from optical data
Article
false
ORIGINAL
0004-637X_746_2_124.pdf
0004-637X_746_2_124.pdf
application/pdf
19049609
https://scholarworks.iu.edu/dspace/bitstream/2022/19085/1/0004-637X_746_2_124.pdf
cf88aa642f1e8ca758b9f54dc0878ff2
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19085/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19085/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_746_2_124.pdf.txt
0004-637X_746_2_124.pdf.txt
Extracted text
text/plain
63435
https://scholarworks.iu.edu/dspace/bitstream/2022/19085/4/0004-637X_746_2_124.pdf.txt
745c72cc8b10dafc9393a138dc8ae835
MD5
4
THUMBNAIL
0004-637X_746_2_124.pdf.jpg
0004-637X_746_2_124.pdf.jpg
IM Thumbnail
image/jpeg
2382
https://scholarworks.iu.edu/dspace/bitstream/2022/19085/5/0004-637X_746_2_124.pdf.jpg
72265e70290659abf2fb050e31e1ed02
MD5
5
2022/19085
oai:scholarworks.iu.edu:2022/19085
2021-10-18 09:39:36.137
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190862021-10-18T14:15:49Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Nakajima, K.
Ouchi, M.
Shimasaku, K.
Ono, Y.
Lee, J.C.
Foucad, S.
Ly, C.
Dale, D.A.
Salim, S.
Finn, R.
Almaini, O.
Okamura, S.
2014-10-30T20:13:38Z
2014-10-30T20:13:38Z
2012
Nakajima, K., Ouchi, M., Shimasaku, K., Ono, Y., Lee, J. C., Foucaud, S., . . . Okamura, S. (2012). Average metallicity and star formation rate of Ly$\alpha$ emitters probed by a triple narrowband survey. Astrophysical Journal, 745(1), 12. http://dx.doi.org/10.1088/0004-637X/745/1/12
http://hdl.handle.net/2022/19086
*Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.
We present the average metallicity and star formation rate (SFR) of $Ly\alpha$ emitters (LAEs) measured from our large-area survey with three narrowband (NB) filters covering the $Ly\alpha, \big[O II\big]\lambda3727$, and $\text{H}\alpha+\big[\text{N} II\big]$ lines of LAEs at $z = 2.2$. We select 919 $z = 2.2$ LAEs from Subaru/Suprime-Cam NB data in conjunction with Magellan/IMACS spectroscopy. Of these LAEs, 561 and 105 are observed with KPNO/NEWFIRM near-infrared NB filters whose central wavelengths are matched to redshifted $\big[\text{O} II\big]$ and $\text{H}\alpha$ nebular lines, respectively. By stacking the near-infrared images of the LAEs, we successfully obtain average nebular-line fluxes of LAEs, the majority of which are too faint to be identified individually by NB imaging or deep spectroscopy. The stacked object has an Hα luminosity of $1.7 × 10^{42} erg s^{–1}$ corresponding to an SFR of $14 M_{\odot} yr6{–1}$. We place, for the first time, a firm lower limit to the average metallicity of LAEs of $Z \gtrsim 0.09 Z_{\odot} \big(2\sigma\big)$ based on the $\big[\text{O} II\big]/\big(\text{H}\alpha+\big[\text{N} II\big]\big)$ index together with photoionization models and empirical relations. This lower limit of metallicity rules out the hypothesis that LAEs, so far observed at $z \sim 2$, are extremely metal-poor $\big(Z < 2 × 10–2 Z_{\odot}\big)$ galaxies at the $4\sigma$ level. This limit is higher than a simple extrapolation of the observed mass-metallicity relation of $z \sim 2$ UV-selected galaxies toward lower masses $\big(5 × 108 M_{\odot}\big)$, but roughly consistent with a recently proposed fundamental mass-metallicity relation when the LAEs' relatively low SFR is taken into account. The $\text{H}\alpha$ and $\text{Ly}\alpha$ luminosities of our NB-selected LAEs indicate that the escape fraction of $\text{Ly}\alpha$ photons is $\sim12%-30%$, much higher than the values derived for other galaxy populations at $z \sim 2$.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:13:38Z
No. of bitstreams: 1
0004-637X_745_1_12.pdf: 2689008 bytes, checksum: 55faa268c8ec58fab048e1437acd6caf (MD5)
Made available in DSpace on 2014-10-30T20:13:38Z (GMT). No. of bitstreams: 1
0004-637X_745_1_12.pdf: 2689008 bytes, checksum: 55faa268c8ec58fab048e1437acd6caf (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/745/1/12
© 2012 The American Astronomical Society
galaxies: abundances
galaxies: evolution
galaxies: formation
galaxies: high-redshift
galaxies: star formation
Average metallicity and star formation rate of Ly$\alpha$ emitters probed by a triple narrowband survey*
Article
true
ORIGINAL
0004-637X_745_1_12.pdf
0004-637X_745_1_12.pdf
application/pdf
2689008
https://scholarworks.iu.edu/dspace/bitstream/2022/19086/1/0004-637X_745_1_12.pdf
55faa268c8ec58fab048e1437acd6caf
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19086/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19086/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_745_1_12.pdf.txt
0004-637X_745_1_12.pdf.txt
Extracted text
text/plain
111705
https://scholarworks.iu.edu/dspace/bitstream/2022/19086/4/0004-637X_745_1_12.pdf.txt
78f90ca543abbe3367a9ef7e6dc8f015
MD5
4
THUMBNAIL
0004-637X_745_1_12.pdf.jpg
0004-637X_745_1_12.pdf.jpg
IM Thumbnail
image/jpeg
2217
https://scholarworks.iu.edu/dspace/bitstream/2022/19086/5/0004-637X_745_1_12.pdf.jpg
f81191a011fd8a9a5041ddb95a952c74
MD5
5
2022/19086
oai:scholarworks.iu.edu:2022/19086
2021-10-18 10:15:49.565
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190872021-10-18T14:16:25Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Salim, S.
Hammer, D.M.
Hornschemeier, A.E.
Smith, R.
Jenkins, L.
Mobasher, B.
Miller, N.
Ferguson, H.
2014-10-30T20:29:57Z
2014-10-30T20:29:57Z
2012
Hammer, D. M., Hornschemeier, A. E., Salim, S., Smith, R., Jenkins, L., Mobasher, B., . . . Ferguson, H. (2012). Deep ultraviolet luminosity functions at the infall region of the coma cluster. Astrophysical Journal, 745(2), 177. http://dx.doi.org/10.1088/0004-637X/745/2/177
http://hdl.handle.net/2022/19087
We have used deep $\textit{GALEX}$ observations at the infall region of the Coma cluster to measure the faintest ultraviolet (UV) luminosity functions (LFs) presented for a rich galaxy cluster thus far. The Coma UV LFs are measured to $M_{UV} = –10.5$ in the $\textit{GALEX}$ FUV and NUV bands, or 3.5 mag fainter than previous studies, and reach the dwarf early-type galaxy population in Coma for the first time. The Schechter faint-end slopes ($\alpha \approx –1.39$ in both $\textit{GALEX}$ bands) are shallower than reported in previous Coma UV LF studies owing to a flatter LF at faint magnitudes. A Gaussian-plus-Schechter model provides a slightly better parameterization of the UV LFs resulting in a faint-end slope of $\alpha \approx –1.15$ in both $\textit{GALEX}$ bands. The two-component model gives faint-end slopes shallower than $\alpha = –1$ (a turnover) for the LFs constructed separately for passive and star-forming galaxies. The UV LFs for star-forming galaxies show a turnover at $M_{UV} \approx –14$ owing to a deficit of dwarf star-forming galaxies in Coma with stellar masses below $M_{*} = 108 M_{\odot}$. A similar turnover is identified in recent UV LFs measured for the Virgo cluster suggesting this may be a common feature of local galaxy clusters, whereas the field UV LFs continue to rise at faint magnitudes. We did not identify an excess of passive galaxies as would be expected if the missing dwarf star-forming galaxies were quenched inside the cluster. In fact, the LFs for both dwarf passive and star-forming galaxies show the same turnover at faint magnitudes. We discuss the possible origin of the missing dwarf star-forming galaxies in Coma and their expected properties based on comparisons to local field galaxies.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:29:57Z
No. of bitstreams: 1
0004-637X_745_2_177.pdf: 1469358 bytes, checksum: 79118d708f0e087148e489d0d2d9efca (MD5)
Made available in DSpace on 2014-10-30T20:29:57Z (GMT). No. of bitstreams: 1
0004-637X_745_2_177.pdf: 1469358 bytes, checksum: 79118d708f0e087148e489d0d2d9efca (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/745/2/177
© 2012 The American Astronomical Society
galaxies: clusters: individual (Coma)
galaxies: dwarf
galaxies: luminosity function, mass function
ultraviolet: galaxies
Deep ultraviolet luminosity functions at the infall region of the coma cluster
Article
false
ORIGINAL
0004-637X_745_2_177.pdf
0004-637X_745_2_177.pdf
application/pdf
1469358
https://scholarworks.iu.edu/dspace/bitstream/2022/19087/1/0004-637X_745_2_177.pdf
79118d708f0e087148e489d0d2d9efca
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19087/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19087/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_745_2_177.pdf.txt
0004-637X_745_2_177.pdf.txt
Extracted text
text/plain
103093
https://scholarworks.iu.edu/dspace/bitstream/2022/19087/4/0004-637X_745_2_177.pdf.txt
48dfcff3ff48abc68bcfe2963dc162ff
MD5
4
THUMBNAIL
0004-637X_745_2_177.pdf.jpg
0004-637X_745_2_177.pdf.jpg
IM Thumbnail
image/jpeg
2340
https://scholarworks.iu.edu/dspace/bitstream/2022/19087/5/0004-637X_745_2_177.pdf.jpg
d523be3ecfa9bc2f7275f673c2e24ff3
MD5
5
2022/19087
oai:scholarworks.iu.edu:2022/19087
2021-10-18 10:16:25.779
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190882021-10-18T14:28:08Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Salim, S.
Lee, J.C.
2014-10-30T20:37:20Z
2014-10-30T20:37:20Z
2012
Salim, S., & Lee, J. C. (2012). Star formation rate distributions: Inadequacy of the Schechter function. Astrophysical Journal, 758(2), 134. http://dx.doi.org/10.1088/0004-637X/758/2/134
http://hdl.handle.net/2022/19088
In this paper, we posit that galaxy luminosity functions (LFs) come in two fundamentally different types depending on whether the luminosity traces galaxy stellar mass or its current star formation rate (SFR). $\textit{Mass function types}$ reflect the older stars and therefore the stellar mass distribution, while $\textit{SFR function types}$ arise from the young stars and hence the distribution of SFRs. Optical and near-infrared LFs are of the mass function type and are well fit by a Schechter function (power law with an exponential cutoff at the bright end). In contrast, LFs of the SFR function type are of a different form, one that cannot be adequately described by a Schechter function. We demonstrate this difference by generating SFR distributions for mock samples of galaxies drawn from a Schechter stellar mass distribution along with established empirical relations between the SFR and stellar mass. Compared with the Schechter function, SFR distributions have a shallower decline at the bright end, which can be traced to the large intrinsic scatter of SFRs at any given stellar mass. A superior description of SFR distributions is given by the "Saunders" function, which combines a power law with a Gaussian at the high end. We show that the Schechter-like appearance of UV and Hα LFs, although they are LFs of SFR function type, results when luminosities are not corrected for dust, or when average statistical corrections are used because individual attenuation measurements are not available. We thus infer that the non-Schechter form of the far-IR LFs is a true reflection of the underlying SFR distribution, rather than the purported artifact of active galactic nucleus contamination.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:37:20Z
No. of bitstreams: 1
0004-637X_758_2_134.pdf: 776078 bytes, checksum: 6c5a470ad828fc8982328c7aef30ad34 (MD5)
Made available in DSpace on 2014-10-30T20:37:20Z (GMT). No. of bitstreams: 1
0004-637X_758_2_134.pdf: 776078 bytes, checksum: 6c5a470ad828fc8982328c7aef30ad34 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/758/2/134
galaxies: evolution
galaxies: fundamental parameters
galaxies: luminosity function, mass function
methods: analytical
methods: numerical
Star formation rate distributions: Inadequacy of the Schechter function
Article
true
ORIGINAL
0004-637X_758_2_134.pdf
0004-637X_758_2_134.pdf
application/pdf
776078
https://scholarworks.iu.edu/dspace/bitstream/2022/19088/1/0004-637X_758_2_134.pdf
6c5a470ad828fc8982328c7aef30ad34
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19088/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19088/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_758_2_134.pdf.txt
0004-637X_758_2_134.pdf.txt
Extracted text
text/plain
85427
https://scholarworks.iu.edu/dspace/bitstream/2022/19088/4/0004-637X_758_2_134.pdf.txt
6d8448f42578d0019a9051c4fcefec8c
MD5
4
THUMBNAIL
0004-637X_758_2_134.pdf.jpg
0004-637X_758_2_134.pdf.jpg
IM Thumbnail
image/jpeg
2208
https://scholarworks.iu.edu/dspace/bitstream/2022/19088/5/0004-637X_758_2_134.pdf.jpg
69c32abb0e582f28f30f8409f5559c72
MD5
5
2022/19088
oai:scholarworks.iu.edu:2022/19088
2021-10-18 10:28:08.323
IUScholarWorks
iusw@indiana.edu
CkJ5IHNpZ25pbmcgYW5kIHN1Ym1pdHRpbmcgdGhpcyBsaWNlbnNlLCB5b3UgKHRoZSBjcmVhdG9yIG9yIGNvcHlyaWdodCBvd25lcikgZ3JhbnQgdG8gSW5kaWFuYSBVbml2ZXJzaXR5IGEgbm9uLWV4Y2x1c2l2ZSwgcGVycGV0dWFsLCBpcnJldm9jYWJsZSByaWdodCB0byByZXByb2R1Y2UsIHRyYW5zbGF0ZSAoYXMgZGVmaW5lZCBiZWxvdyksIGFuZC9vciBkaXN0cmlidXRlIHlvdXIgc3VibWlzc2lvbiAoaW5jbHVkaW5nIHRoZSBhYnN0cmFjdCkgd29ybGR3aWRlIGluIHByaW50IGFuZCBlbGVjdHJvbmljIGZvcm1hdCBhbmQgaW4gYW55IG1lZGl1bSwgaW5jbHVkaW5nIGJ1dCBub3QgbGltaXRlZCB0byBhdWRpbyBvciB2aWRlby4KCllvdSBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXksIHdpdGhvdXQgY2hhbmdpbmcgdGhlIGNvbnRlbnQsIHRyYW5zbGF0ZSB0aGUgc3VibWlzc2lvbiB0byBhbnkgbWVkaXVtIG9yIGZvcm1hdCBmb3IgcHJlc2VydmF0aW9uIG9yIGFjY2VzcywgYW5kIHByb3ZpZGUgYmFzaWMgbWV0YWRhdGEgdGhhdCBkZXNjcmliZXMgdGhlIGNvbnRlbnRzIGZvciBkaXNjb3ZlcnkuCgpZb3UgYWxzbyBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXkga2VlcCBtb3JlIHRoYW4gb25lIGNvcHkgb2YgdGhpcyBzdWJtaXNzaW9uIGZvciBzZWN1cml0eSwgYmFjay11cCBhbmQgcHJlc2VydmF0aW9uLgoKWW91IHJlcHJlc2VudCB0aGF0IHRoZSBzdWJtaXNzaW9uIGlzIHlvdXIgb3JpZ2luYWwgd29yaywgYW5kIHRoYXQgeW91IGhhdmUgdGhlIHJpZ2h0IHRvIGdyYW50IHRoZSByaWdodHMgY29udGFpbmVkIGluIHRoaXMgbGljZW5zZS4gWW91IGFsc28gcmVwcmVzZW50IHRoYXQgeW91ciBzdWJtaXNzaW9uIGRvZXMgbm90LCB0byB0aGUgYmVzdCBvZiB5b3VyIGtub3dsZWRnZSwgaW5mcmluZ2UgdXBvbiBhbnlvbmUncyBjb3B5cmlnaHQuCgpJZiB0aGUgc3VibWlzc2lvbiBjb250YWlucyBtYXRlcmlhbCBmb3Igd2hpY2ggeW91IGRvIG5vdCBob2xkIGNvcHlyaWdodCwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIG9idGFpbmVkIHRoZSB1bnJlc3RyaWN0ZWQgcGVybWlzc2lvbiBvZiB0aGUgY29weXJpZ2h0IG93bmVyIHRvIGdyYW50IEluZGlhbmEgVW5pdmVyc2l0eSB0aGUgcmlnaHRzIHJlcXVpcmVkIGJ5IHRoaXMgbGljZW5zZSwgYW5kIHRoYXQgc3VjaCB0aGlyZC1wYXJ0eSBvd25lZCBtYXRlcmlhbCBpcyBjbGVhcmx5IGlkZW50aWZpZWQgYW5kIGFja25vd2xlZGdlZCB3aXRoaW4gdGhlIHRleHQgb3IgY29udGVudCBvZiB0aGUgc3VibWlzc2lvbi4KCklmIHRoZSBzdWJtaXNzaW9uIGlzIGJhc2VkIHVwb24gd29yayB0aGF0IGhhcyBiZWVuIHNwb25zb3JlZCBvciBzdXBwb3J0ZWQgYnkgYW4gYWdlbmN5IG9yIG9yZ2FuaXphdGlvbiBvdGhlciB0aGFuIEluZGlhbmEgVW5pdmVyc2l0eSwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIGZ1bGZpbGxlZCBhbnkgcmlnaHQgb2YgcmV2aWV3IG9yIG90aGVyIG9ibGlnYXRpb25zIHJlcXVpcmVkIGJ5IHN1Y2ggY29udHJhY3Qgb3IgYWdyZWVtZW50LgoKSW5kaWFuYSBVbml2ZXJzaXR5IHdpbGwgY2xlYXJseSBpZGVudGlmeSB5b3VyIG5hbWUgYXMgdGhlIGNyZWF0b3IgYW5kL29yIGNvcHlyaWdodCBvd25lciBvZiB0aGUgc3VibWlzc2lvbiwgYW5kIHdpbGwgbm90IG1ha2UgYW55IGFsdGVyYXRpb24sIG90aGVyIHRoYW4gYXMgYWxsb3dlZCBieSB0aGlzIGxpY2Vuc2UsIHRvIHlvdXIgc3VibWlzc2lvbi4gV2UgYWdyZWUgdG8gbm90IG1ha2UgYXZhaWxhYmxlIGFueSBmaWxlcyB0aGF0IGFyZSBlbWJhcmdvZWQgdW50aWwgdGhlIGVtYmFyZ28gaGFzIGV4cGlyZWQuCgpJZiB5b3UgYXJlIHN1Ym1pdHRpbmcgdGhpcyBpdGVtIG9uIGJlaGFsZiBvZiB0aGUgcmlnaHRzIGhvbGRlciwgeW91IG11c3QgaGF2ZSB0aGUgcmlnaHRzIG93bmVyJ3Mgd3JpdHRlbiBwZXJtaXNzaW9uIHRvIGFjY2VwdCB0aGlzIGxpY2Vuc2Ugb24gaGlzL2hlciBiZWhhbGYuCgo=
oai:scholarworks.iu.edu:2022/190892021-10-18T14:28:39Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Cooper, M.C.
Yan, R.
Dickinson, M.
Juneau, S.
Lotz, J.M.
Newman, J.A.
Papovich, C.
Salim, S.
Walth, G.
Weiner, B.J.
Willmer, C.N.A.
2014-10-30T20:44:28Z
2014-10-30T20:44:28Z
2012
Cooper, M. C., Yan, R., Dickinson, M., Juneau, S., Lotz, J. M., Newman, J. A., . . . Willmer, C. N. A. (2012). The arizona CDFS environment survey (ACES): A Magellan/IMACS spectroscopic survey of the chandra deep field-south. Monthly Notices of the Royal Astronomical Society, 425(3), 2116-2127. http://dx.doi.org/10.1111/j.1365-2966.2012.21524.x
http://hdl.handle.net/2022/19089
*This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
We present the Arizona CDFS Environment Survey (ACES), a recently completed spectroscopic redshift survey of the Chandra Deep Field-South (CDFS) conducted using the Inamori-Magellan Areal Camera and Spectrograph on the Magellan-Baade telescope. In total, the survey targeted 7277 unique sources down to a limiting magnitude of $R_{AB} = 24.1$, yielding 5080 secure redshifts across the $\sim30 arcmin × 30 arcmin$ extended CDFS region. The ACES data set delivers a significant increase to both the spatial coverage and the sampling density of the spectroscopic observations in the field. Combined with previously published spectroscopic redshifts, ACES now creates a highly complete survey of the galaxy population at $R < 23$, enabling the local galaxy density (or environment) on relatively small scales ($\sim 1 \text{Mpc}$) to be measured at $z < 1$ in one of the most heavily studied and data-rich fields in the sky. Here, we describe the motivation, design and implementation of the survey and present a preliminary redshift and environment catalogue. In addition, we utilize the ACES spectroscopic redshift catalogue to assess the quality of photometric redshifts from both the COMBO-17 and Multiwavelength Survey by Yale-Chile imaging surveys of the CDFS.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:44:28Z
No. of bitstreams: 1
MNRAS-2012-Cooper-2116-27.pdf: 3514818 bytes, checksum: b12b50ead13c47837da602947e8f1f67 (MD5)
Made available in DSpace on 2014-10-30T20:44:28Z (GMT). No. of bitstreams: 1
MNRAS-2012-Cooper-2116-27.pdf: 3514818 bytes, checksum: b12b50ead13c47837da602947e8f1f67 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1111/j.1365-2966.2012.21524.x
© 2012 The Authors
Catalogues
Galaxies: distances and redshifts
Surveys
The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South*
Article
true
ORIGINAL
MNRAS-2012-Cooper-2116-27.pdf
MNRAS-2012-Cooper-2116-27.pdf
application/pdf
3514818
https://scholarworks.iu.edu/dspace/bitstream/2022/19089/1/MNRAS-2012-Cooper-2116-27.pdf
b12b50ead13c47837da602947e8f1f67
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19089/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19089/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
MNRAS-2012-Cooper-2116-27.pdf.txt
MNRAS-2012-Cooper-2116-27.pdf.txt
Extracted text
text/plain
66751
https://scholarworks.iu.edu/dspace/bitstream/2022/19089/4/MNRAS-2012-Cooper-2116-27.pdf.txt
b3cb513b139f32e2473f007bfa1adb18
MD5
4
THUMBNAIL
MNRAS-2012-Cooper-2116-27.pdf.jpg
MNRAS-2012-Cooper-2116-27.pdf.jpg
IM Thumbnail
image/jpeg
3323
https://scholarworks.iu.edu/dspace/bitstream/2022/19089/5/MNRAS-2012-Cooper-2116-27.pdf.jpg
ddabcf7ac89892188886df754876441b
MD5
5
2022/19089
oai:scholarworks.iu.edu:2022/19089
2021-10-18 10:28:39.985
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190902021-10-18T14:28:01Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Fang, J.J.
Faber, S.M.
Salim, S.
Graves, G.J.
Rich, R.M.
2014-10-30T20:50:44Z
2014-10-30T20:50:44Z
2012
Fang, J. J., Faber, S. M., Salim, S., Graves, G. J., & Rich, R. M. (2012). The slow death (or rebirth?) of extended star formation in $z \sim 0.1$ green valley early-type galaxies. Astrophysical Journal, 761(1), 23. http://dx.doi.org/10.1088/0004-637X/761/1/23
http://hdl.handle.net/2022/19090
UV observations in the local universe have uncovered a population of early-type galaxies with UV flux consistent with low-level recent or ongoing star formation. Understanding the origin of such star formation remains an open issue. We present resolved UV-optical photometry of a sample of 19 Sloan Digital Sky Survey (SDSS) early-type galaxies at $z \sim 0.1$ drawn from the sample originally selected by Salim & Rich to lie in the bluer part of the green valley in the UV-optical color-magnitude diagram as measured by the $\textit{Galaxy Evolution Explorer (GALEX)}$. Utilizing high-resolution $\textit{Hubble Space Telescope (HST)}$ far-UV imaging provides unique insight into the distribution of UV light in these galaxies, which we call "extended star-forming early-type galaxies" (ESF-ETGs) because of extended UV emission that is indicative of recent star formation. The UV-optical color profiles of all ESF-ETGs show red centers and blue outer parts. Their outer colors require the existence of a significant underlying population of older stars in the UV-bright regions. An analysis of stacked SDSS spectra reveals weak LINER-like emission in their centers. Using a cross-matched SDSS DR7/$GALEX$ GR6 catalog, we search for other green valley galaxies with similar properties to these ESF-ETGs and estimate that $\approx 13%$ of dust-corrected green valley galaxies of similar stellar mass and UV-optical color are likely ESF-candidates, i.e., ESF-ETGs are not rare. Our results are consistent with star formation that is gradually declining in existing disks, i.e., the ESF-ETGs are evolving onto the red sequence for the first time, or with rejuvenated star formation due to accreted gas in older disks provided that the gas does not disrupt the structure of the galaxy and the resulting star formation is not too recent and bursty. ESF-ETGs may typify an important subpopulation of galaxies that can linger in the green valley for up to several Gyrs, based on their resemblance to nearby gas-rich green valley galaxies with low-level ongoing star formation.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:50:44Z
No. of bitstreams: 1
0004-637X_761_1_23.pdf: 1197083 bytes, checksum: e86294c45b83e157c0adde5f6faccce6 (MD5)
Made available in DSpace on 2014-10-30T20:50:44Z (GMT). No. of bitstreams: 1
0004-637X_761_1_23.pdf: 1197083 bytes, checksum: e86294c45b83e157c0adde5f6faccce6 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/761/1/23
© 2012 The American Astronomical Society
galaxies: elliptical and lenticular, cD
galaxies: evolution
galaxies: photometry
ultraviolet: galaxies
The slow death (or rebirth?) of extended star formation in $z \sim 0.1$ green valley early-type galaxies
Article
true
ORIGINAL
0004-637X_761_1_23.pdf
0004-637X_761_1_23.pdf
application/pdf
1197083
https://scholarworks.iu.edu/dspace/bitstream/2022/19090/1/0004-637X_761_1_23.pdf
e86294c45b83e157c0adde5f6faccce6
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19090/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19090/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_761_1_23.pdf.txt
0004-637X_761_1_23.pdf.txt
Extracted text
text/plain
104651
https://scholarworks.iu.edu/dspace/bitstream/2022/19090/4/0004-637X_761_1_23.pdf.txt
440c75ae876c8b6ab10918aae3da3f04
MD5
4
THUMBNAIL
0004-637X_761_1_23.pdf.jpg
0004-637X_761_1_23.pdf.jpg
IM Thumbnail
image/jpeg
2217
https://scholarworks.iu.edu/dspace/bitstream/2022/19090/5/0004-637X_761_1_23.pdf.jpg
ed0b39f7802e70ce66009386f8610c78
MD5
5
2022/19090
oai:scholarworks.iu.edu:2022/19090
2021-10-18 10:28:01.053
IUScholarWorks
iusw@indiana.edu
CkJ5IHNpZ25pbmcgYW5kIHN1Ym1pdHRpbmcgdGhpcyBsaWNlbnNlLCB5b3UgKHRoZSBjcmVhdG9yIG9yIGNvcHlyaWdodCBvd25lcikgZ3JhbnQgdG8gSW5kaWFuYSBVbml2ZXJzaXR5IGEgbm9uLWV4Y2x1c2l2ZSwgcGVycGV0dWFsLCBpcnJldm9jYWJsZSByaWdodCB0byByZXByb2R1Y2UsIHRyYW5zbGF0ZSAoYXMgZGVmaW5lZCBiZWxvdyksIGFuZC9vciBkaXN0cmlidXRlIHlvdXIgc3VibWlzc2lvbiAoaW5jbHVkaW5nIHRoZSBhYnN0cmFjdCkgd29ybGR3aWRlIGluIHByaW50IGFuZCBlbGVjdHJvbmljIGZvcm1hdCBhbmQgaW4gYW55IG1lZGl1bSwgaW5jbHVkaW5nIGJ1dCBub3QgbGltaXRlZCB0byBhdWRpbyBvciB2aWRlby4KCllvdSBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXksIHdpdGhvdXQgY2hhbmdpbmcgdGhlIGNvbnRlbnQsIHRyYW5zbGF0ZSB0aGUgc3VibWlzc2lvbiB0byBhbnkgbWVkaXVtIG9yIGZvcm1hdCBmb3IgcHJlc2VydmF0aW9uIG9yIGFjY2VzcywgYW5kIHByb3ZpZGUgYmFzaWMgbWV0YWRhdGEgdGhhdCBkZXNjcmliZXMgdGhlIGNvbnRlbnRzIGZvciBkaXNjb3ZlcnkuCgpZb3UgYWxzbyBhZ3JlZSB0aGF0IEluZGlhbmEgVW5pdmVyc2l0eSBtYXkga2VlcCBtb3JlIHRoYW4gb25lIGNvcHkgb2YgdGhpcyBzdWJtaXNzaW9uIGZvciBzZWN1cml0eSwgYmFjay11cCBhbmQgcHJlc2VydmF0aW9uLgoKWW91IHJlcHJlc2VudCB0aGF0IHRoZSBzdWJtaXNzaW9uIGlzIHlvdXIgb3JpZ2luYWwgd29yaywgYW5kIHRoYXQgeW91IGhhdmUgdGhlIHJpZ2h0IHRvIGdyYW50IHRoZSByaWdodHMgY29udGFpbmVkIGluIHRoaXMgbGljZW5zZS4gWW91IGFsc28gcmVwcmVzZW50IHRoYXQgeW91ciBzdWJtaXNzaW9uIGRvZXMgbm90LCB0byB0aGUgYmVzdCBvZiB5b3VyIGtub3dsZWRnZSwgaW5mcmluZ2UgdXBvbiBhbnlvbmUncyBjb3B5cmlnaHQuCgpJZiB0aGUgc3VibWlzc2lvbiBjb250YWlucyBtYXRlcmlhbCBmb3Igd2hpY2ggeW91IGRvIG5vdCBob2xkIGNvcHlyaWdodCwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIG9idGFpbmVkIHRoZSB1bnJlc3RyaWN0ZWQgcGVybWlzc2lvbiBvZiB0aGUgY29weXJpZ2h0IG93bmVyIHRvIGdyYW50IEluZGlhbmEgVW5pdmVyc2l0eSB0aGUgcmlnaHRzIHJlcXVpcmVkIGJ5IHRoaXMgbGljZW5zZSwgYW5kIHRoYXQgc3VjaCB0aGlyZC1wYXJ0eSBvd25lZCBtYXRlcmlhbCBpcyBjbGVhcmx5IGlkZW50aWZpZWQgYW5kIGFja25vd2xlZGdlZCB3aXRoaW4gdGhlIHRleHQgb3IgY29udGVudCBvZiB0aGUgc3VibWlzc2lvbi4KCklmIHRoZSBzdWJtaXNzaW9uIGlzIGJhc2VkIHVwb24gd29yayB0aGF0IGhhcyBiZWVuIHNwb25zb3JlZCBvciBzdXBwb3J0ZWQgYnkgYW4gYWdlbmN5IG9yIG9yZ2FuaXphdGlvbiBvdGhlciB0aGFuIEluZGlhbmEgVW5pdmVyc2l0eSwgeW91IHJlcHJlc2VudCB0aGF0IHlvdSBoYXZlIGZ1bGZpbGxlZCBhbnkgcmlnaHQgb2YgcmV2aWV3IG9yIG90aGVyIG9ibGlnYXRpb25zIHJlcXVpcmVkIGJ5IHN1Y2ggY29udHJhY3Qgb3IgYWdyZWVtZW50LgoKSW5kaWFuYSBVbml2ZXJzaXR5IHdpbGwgY2xlYXJseSBpZGVudGlmeSB5b3VyIG5hbWUgYXMgdGhlIGNyZWF0b3IgYW5kL29yIGNvcHlyaWdodCBvd25lciBvZiB0aGUgc3VibWlzc2lvbiwgYW5kIHdpbGwgbm90IG1ha2UgYW55IGFsdGVyYXRpb24sIG90aGVyIHRoYW4gYXMgYWxsb3dlZCBieSB0aGlzIGxpY2Vuc2UsIHRvIHlvdXIgc3VibWlzc2lvbi4gV2UgYWdyZWUgdG8gbm90IG1ha2UgYXZhaWxhYmxlIGFueSBmaWxlcyB0aGF0IGFyZSBlbWJhcmdvZWQgdW50aWwgdGhlIGVtYmFyZ28gaGFzIGV4cGlyZWQuCgpJZiB5b3UgYXJlIHN1Ym1pdHRpbmcgdGhpcyBpdGVtIG9uIGJlaGFsZiBvZiB0aGUgcmlnaHRzIGhvbGRlciwgeW91IG11c3QgaGF2ZSB0aGUgcmlnaHRzIG93bmVyJ3Mgd3JpdHRlbiBwZXJtaXNzaW9uIHRvIGFjY2VwdCB0aGlzIGxpY2Vuc2Ugb24gaGlzL2hlciBiZWhhbGYuCgo=
oai:scholarworks.iu.edu:2022/190912021-10-18T14:28:48Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Wardell, B.
Vega, I.
Thornburg, J.
Diener, P.
2014-10-30T20:57:43Z
2014-10-30T20:57:43Z
2012
Wardell, B., Vega, I., Thornburg, J., & Diener, P. (2012). Generic effective source for scalar self-force calculations. Physical Review D - Particles, Fields, Gravitation and Cosmology, 85(10), 104044. http://dx.doi.org/10.1103/PhysRevD.85.104044
http://hdl.handle.net/2022/19091
A leading approach to the modeling of extreme mass ratio inspirals involves the treatment of the smaller mass as a point particle and the computation of a regularized self-force acting on that particle. In turn, this computation requires knowledge of the regularized retarded field generated by the particle. A direct calculation of this regularized field may be achieved by replacing the point particle with an effective source and solving directly a wave equation for the regularized field. This has the advantage that all quantities are finite and require no further regularization. In this work, we present a method for computing an effective source which is finite and continuous everywhere, and which is valid for a scalar point particle in arbitrary geodesic motion in an arbitrary background spacetime. We explain in detail various technical and practical considerations that underlie its use in several numerical self-force calculations. We consider as examples the cases of a particle in a circular orbit about Schwarzschild and Kerr black holes, and also the case of a particle following a generic timelike geodesic about a highly spinning Kerr black hole. We provide numerical C code for computing an effective source for various orbital configurations about Schwarzschild and Kerr black holes.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-10-30T20:57:43Z
No. of bitstreams: 1
PhysRevD.85.104044.pdf: 1905117 bytes, checksum: fc0332f3b5ea2068e8391771170cc822 (MD5)
Made available in DSpace on 2014-10-30T20:57:43Z (GMT). No. of bitstreams: 1
PhysRevD.85.104044.pdf: 1905117 bytes, checksum: fc0332f3b5ea2068e8391771170cc822 (MD5)
Previous issue date: 2012
en_US
American Physical Society
https://doi.org/10.1103/PhysRevD.85.104044
© 2012 American Physical Society
Generic effective source for scalar self-force calculations
Article
true
ORIGINAL
PhysRevD.85.104044.pdf
PhysRevD.85.104044.pdf
application/pdf
1905117
https://scholarworks.iu.edu/dspace/bitstream/2022/19091/1/PhysRevD.85.104044.pdf
fc0332f3b5ea2068e8391771170cc822
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19091/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
thornburg_jonathan_license_2012.txt
thornburg_jonathan_license_2012.txt
text/plain
4477
https://scholarworks.iu.edu/dspace/bitstream/2022/19091/3/thornburg_jonathan_license_2012.txt
722fbacae76f718f5f7fecd33b9e8548
MD5
3
TEXT
PhysRevD.85.104044.pdf.txt
PhysRevD.85.104044.pdf.txt
Extracted text
text/plain
93894
https://scholarworks.iu.edu/dspace/bitstream/2022/19091/4/PhysRevD.85.104044.pdf.txt
1f24aa9821267cd6dbe7edf788dbc319
MD5
4
THUMBNAIL
PhysRevD.85.104044.pdf.jpg
PhysRevD.85.104044.pdf.jpg
IM Thumbnail
image/jpeg
2001
https://scholarworks.iu.edu/dspace/bitstream/2022/19091/5/PhysRevD.85.104044.pdf.jpg
dea646f976fabfa7bce90f9eaabe9db0
MD5
5
2022/19091
oai:scholarworks.iu.edu:2022/19091
2021-10-18 10:28:48.216
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/190992021-10-18T14:28:52Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Weisz, D.R.
Johnson, B.D.
Johnson, L.C.
Skillman, E.D.
Lee, J.C.
Kennicutt, R.C.
Calzetti, D.
Van Zee, L.
Bothwell, M.S.
Dalcanton, J.J.
Dale, D.A.
Williams, B.F.
2014-11-03T18:04:17Z
2014-11-03T18:04:17Z
2012
Weisz, D. R., Johnson, B. D., Johnson, L. C., Skillman, E. D., Lee, J. C., Kennicutt, R. C., . . . Williams, B. F. (2012). Modeling the effects of star formation histories on H$\alpha$ and ultraviolet fluxes in nearby dwarf galaxies. Astrophysical Journal, 744(1), 44. http://dx.doi.org/10.1088/0004-637X/744/1/44
http://hdl.handle.net/2022/19099
We consider the effects of non-constant star formation histories (SFHs) on $\text{H}\alpha$ and GALEX far-ultraviolet (FUV) star formation rate (SFR) indicators. Under the assumption of a fully populated Chabrier initial mass function (IMF), we compare the distribution of $\text{H}\alpha$-to-FUV flux ratios from ~1500 simple, periodic model SFHs with observations of 185 galaxies from the $\textit{Spitzer}$ Local Volume Legacy survey. We find a set of SFH models that are well matched to the data, such that more massive galaxies are best characterized by nearly constant SFHs, while low-mass systems experience burst amplitudes of ~30 (i.e., an increase in the SFR by a factor of 30 over the SFR during the inter-burst period), burst durations of tens of Myr, and periods of ~250 Myr; these SFHs are broadly consistent with the increased stochastic star formation expected in systems with lower SFRs. We analyze the predicted temporal evolution of galaxy stellar mass, R-band surface brightness, $\text{H}\alpha$-derived SFR, and blue luminosity, and find that they provide a reasonable match to observed flux distributions. We find that our model SFHs are generally able to reproduce both the observed systematic decline and increased scatter in $\text{H}\alpha$-to-FUV ratios toward low-mass systems, without invoking other physical mechanisms. We also compare our predictions with those from the Integrated Galactic IMF theory with a constant SFR. We find that while both predict a systematic decline in the observed ratios, only the time variable SFH models are capable of producing the observed population of low-mass galaxies $\big(M_{*} \lesssim 10^{7} M_{\odot}\big)$ with normal $\text{H}\alpha$-to-FUV ratios. These results demonstrate that a variable IMF alone has difficulty explaining the observed scatter in the $\text{H}\alpha$-to-FUV ratios. We conclude by considering the limitations of the model SFHs and discuss the use of additional empirical constraints to improve future SFH modeling efforts.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T18:04:17Z
No. of bitstreams: 1
0004-637X_744_1_44.pdf: 1519319 bytes, checksum: 5bf23ab3f6dc84b43e79fd62f99fd0cc (MD5)
Made available in DSpace on 2014-11-03T18:04:17Z (GMT). No. of bitstreams: 1
0004-637X_744_1_44.pdf: 1519319 bytes, checksum: 5bf23ab3f6dc84b43e79fd62f99fd0cc (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/744/1/44
© 2012 The American Astronomical Society
galaxies: dwarf
galaxies: evolution
galaxies: formation
galaxies: star formation
Modeling the effects of star formation histories on H$\alpha$ and ultraviolet fluxes in nearby dwarf galaxies
Article
true
ORIGINAL
0004-637X_744_1_44.pdf
0004-637X_744_1_44.pdf
application/pdf
1519319
https://scholarworks.iu.edu/dspace/bitstream/2022/19099/1/0004-637X_744_1_44.pdf
5bf23ab3f6dc84b43e79fd62f99fd0cc
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19099/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
vanzee_liese_license_2012.txt
vanzee_liese_license_2012.txt
text/plain
4661
https://scholarworks.iu.edu/dspace/bitstream/2022/19099/3/vanzee_liese_license_2012.txt
85956b2c821b605a4353c066560a449f
MD5
3
TEXT
0004-637X_744_1_44.pdf.txt
0004-637X_744_1_44.pdf.txt
Extracted text
text/plain
79997
https://scholarworks.iu.edu/dspace/bitstream/2022/19099/4/0004-637X_744_1_44.pdf.txt
c6bb4a4e13dcee41ddcaa9528f91e5d1
MD5
4
THUMBNAIL
0004-637X_744_1_44.pdf.jpg
0004-637X_744_1_44.pdf.jpg
IM Thumbnail
image/jpeg
2308
https://scholarworks.iu.edu/dspace/bitstream/2022/19099/5/0004-637X_744_1_44.pdf.jpg
bee046e1edd4635ae972fa17e797d1fd
MD5
5
2022/19099
oai:scholarworks.iu.edu:2022/19099
2021-10-18 10:28:52.069
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/191002021-10-18T14:06:45Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Kellar, J.A.
Salzer, J.J.
Wegner, G.
Gronwall, C.
Williams, A.
2014-11-03T18:11:57Z
2014-11-03T18:11:57Z
2012
Kellar, J. A., Salzer, J. J., Wegner, G., Gronwall, C., & Williams, A. (2012). Hα dots: A catalog of faint emission-line objects discovered in narrowband images. Astronomical Journal, 143(6), 145. http://dx.doi.org/10.1088/0004-6256/143/6/145
http://hdl.handle.net/2022/19100
During a wide-field narrowband $\text{H}\alpha$ imaging survey, we noted the presence of numerous isolated emission-line point sources in the data. These objects could represent ultra-low-luminosity galaxies at low-redshift (detection via $\text{H}\alpha$), isolated extragalactic H II regions associated with the galaxy targeted by the original observation, or background galaxies or QSOs where strong emission lines (most often [O III] $\lambda$ 5007) redshift into our narrowband filter. We have carried out a systematic search for these "$\text{H}\alpha$ dots" in over 200 15 × 15 arcmin fields. To date we have cataloged 61 candidate emission-line sources in roughly 11.7 deg$^{2}$. The sample has a median R magnitude of 19.5, and detects objects as faint as $R$ = 22.6. Follow-up spectroscopy reveals that ~85% of the candidates are bona fide emission-line objects, with roughly 60% of the real sources being lower-redshift objects (detection via $\text{H}\alpha$) and 40% being higher-redshift objects detected via [O III] emission or some other emission line. Here we present the results of our initial survey and follow-up spectroscopy. We use our sample to study the properties (including star-formation rates and metal abundances) of low-luminosity star-forming galaxies in the nearby universe and of low-metallicity star-forming galaxies at $z \approx 0.33$.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T18:11:57Z
No. of bitstreams: 1
1538-3881_143_6_145.pdf: 2565038 bytes, checksum: 800cbfcad0160e0991278e78eae84203 (MD5)
Made available in DSpace on 2014-11-03T18:11:57Z (GMT). No. of bitstreams: 1
1538-3881_143_6_145.pdf: 2565038 bytes, checksum: 800cbfcad0160e0991278e78eae84203 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-6256/143/6/145
© 2012 The American Astronomical Society
galaxies: abundances
galaxies: dwarf
galaxies: starburst
surveys
$\text{H}\alpha$ dots: A catalog of faint emission-line objects discovered in narrowband images
Article
false
ORIGINAL
1538-3881_143_6_145.pdf
1538-3881_143_6_145.pdf
application/pdf
2565038
https://scholarworks.iu.edu/dspace/bitstream/2022/19100/1/1538-3881_143_6_145.pdf
800cbfcad0160e0991278e78eae84203
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19100/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salzer_john_license_2012.txt
salzer_john_license_2012.txt
text/plain
4581
https://scholarworks.iu.edu/dspace/bitstream/2022/19100/3/salzer_john_license_2012.txt
9b1d8f3a4f663a2c76c814bc29c27006
MD5
3
TEXT
1538-3881_143_6_145.pdf.txt
1538-3881_143_6_145.pdf.txt
Extracted text
text/plain
103490
https://scholarworks.iu.edu/dspace/bitstream/2022/19100/4/1538-3881_143_6_145.pdf.txt
1b286ba5db26b5c967f3babc4d466fa4
MD5
4
THUMBNAIL
1538-3881_143_6_145.pdf.jpg
1538-3881_143_6_145.pdf.jpg
IM Thumbnail
image/jpeg
2395
https://scholarworks.iu.edu/dspace/bitstream/2022/19100/5/1538-3881_143_6_145.pdf.jpg
59785d4dc0b17c89d9b04203606b203d
MD5
5
2022/19100
oai:scholarworks.iu.edu:2022/19100
2021-10-18 10:06:45.354
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/191032021-10-18T14:12:08Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Berg, D.A.
Skillman, E.D.
Marble, A.R.
Van Zee, L.
Engelbracht, C.W.
Lee, J.C.
Kennicutt, R.C.
Calzetti, D.
Dale, D.A.
Johnson, B.D.
2014-11-03T18:42:05Z
2014-11-03T18:42:05Z
2012
Berg, D. A., Skillman, E. D., Marble, A. R., Van Zee, L., Engelbracht, C. W., Lee, J. C., . . . Johnson, B. D. (2012). Direct oxygen abundances for low-luminosity LVL galaxies. Astrophysical Journal, 754(2), 98. http://dx.doi.org/10.1088/0004-637X/754/2/98
http://hdl.handle.net/2022/19103
We present MMT spectroscopic observations of H II regions in 42 low luminosity galaxies in the Spitzer Local Volume Legacy survey. For 31 of the 42 galaxies in our sample, we were able to measure the temperature sensitive [O III] $\lambda$4363 line at a strength of $4\sigma$ or greater, and thus determine oxygen abundances using the "direct" method. Our results provide the first "direct" estimates of oxygen abundance for 19 of these galaxies. "Direct" oxygen abundances were compared to $B$-band luminosities, 4.5 $\mu$m luminosities, and stellar masses in order to characterize the luminosity-metallicity and mass-metallicity relationships at low luminosity. We present and analyze a "Combined Select" sample composed of 38 objects (drawn from a sub-set of our parent sample and the literature) with "direct" oxygen abundances and reliable distance determinations (based on the tip of the red giant branch or Cepheid variables). Consistent with previous studies, the $B$ band and 4.5 $\mu$m luminosity-metallicity relationships for the 38 objects were found to be$12 + log(O/H) = (6.27 \pm 0.21) + (- 0.11 \pm 0.01)M_{B}$and$12+log(O/H) = (6.10 \pm 0.21) + (- 0.10 \pm 0.01)M_{[4.5]}$with dispersions of $\sigma$ = 0.15 and 0.14, respectively. The slopes of the optical and near-IR L-Z relationships have been reported to be different for galaxies with luminosities greater than that of the LMC. However, the similarity of the slopes of the optical and near-IR L-Z relationships for our sample probably reflects little influence by dust extinction in the low luminosity galaxies. For this sample, we derive a mass-metallicity relationship of $12 + log\big(O/H\big) = \big(5.61 \pm 0.24\big) + \big(0.29 \pm 0.03\big)log \big(M_{\star}\big)$, which agrees with previous studies; however, the dispersion ($\sigma$ = 0.15) is not significantly lower than that of the L-Z relationships. Because of the low dispersions in these relationships, if an accurate distance is available, the luminosity of a low luminosity galaxy is often a better indicator of metallicity than that derived using certain "strong-line" methods, so significant departures from the L-Z relationships may indicate that caution is prudent in such cases. With these new "direct" metallicities we also revisit the 70/160 $\mu$m color metallicity relationship. Additionally, we examine N/O abundance trends with respect to oxygen abundance and B - V color. We find a positive correlation between N/O ratio and B - V color for $0.05 \lesssim B - V \lesssim 0.75: log (N/O) = (1.18 \pm 0.9\big) × (B - V) + (- 1.92 \pm 0.08)$, with a dispersion of $\sigma$ = 0.14, which is in agreement with previous studies.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T18:42:05Z
No. of bitstreams: 1
0004-637X_754_2_98.pdf: 1816598 bytes, checksum: 985d7f83652664ac4c2c54af287ae0fa (MD5)
Made available in DSpace on 2014-11-03T18:42:05Z (GMT). No. of bitstreams: 1
0004-637X_754_2_98.pdf: 1816598 bytes, checksum: 985d7f83652664ac4c2c54af287ae0fa (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/754/2/98
© 2012 The American Astronomical Society
galaxies: abundances
galaxies: dwarf
galaxies: evolution
Direct oxygen abundances for low-luminosity LVL galaxies
Article
false
ORIGINAL
0004-637X_754_2_98.pdf
0004-637X_754_2_98.pdf
application/pdf
1816598
https://scholarworks.iu.edu/dspace/bitstream/2022/19103/1/0004-637X_754_2_98.pdf
985d7f83652664ac4c2c54af287ae0fa
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19103/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
vanzee_liese_license_2012.txt
vanzee_liese_license_2012.txt
text/plain
4661
https://scholarworks.iu.edu/dspace/bitstream/2022/19103/3/vanzee_liese_license_2012.txt
85956b2c821b605a4353c066560a449f
MD5
3
TEXT
0004-637X_754_2_98.pdf.txt
0004-637X_754_2_98.pdf.txt
Extracted text
text/plain
154756
https://scholarworks.iu.edu/dspace/bitstream/2022/19103/4/0004-637X_754_2_98.pdf.txt
b82293ca003e1a6b4225f74ea238b684
MD5
4
THUMBNAIL
0004-637X_754_2_98.pdf.jpg
0004-637X_754_2_98.pdf.jpg
IM Thumbnail
image/jpeg
2267
https://scholarworks.iu.edu/dspace/bitstream/2022/19103/5/0004-637X_754_2_98.pdf.jpg
26917494e321d3ee9c77e80c1a3a6334
MD5
5
2022/19103
oai:scholarworks.iu.edu:2022/19103
2021-10-18 10:12:08.559
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/191072021-10-18T14:14:58Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Young, M.D.
Dowell, J.L.
Rhode, K.L.
2014-11-03T19:34:00Z
2014-11-03T19:34:00Z
2012
Young, M. D., Dowell, J. L., & Rhode, K. L. (2012). Globular cluster systems of spiral and S0 galaxies: Results from WIYN imaging of NGC1023, NGC1055, NGC7332, and NGC7339. Astronomical Journal, 144(4), 103. http://dx.doi.org/10.1088/0004-6256/144/4/103
http://hdl.handle.net/2022/19107
We present results from a study of the globular cluster (GC) systems of four spiral and S0 galaxies imaged as part of an ongoing wide-field survey of the GC systems of giant galaxies. The target galaxies - the SB0 galaxy NGC1023, the SBb galaxy NGC1055, and an isolated pair comprised of the Sbc galaxy NGC7339 and the S0 galaxy NGC7332 - were observed in BVR filters with the WIYN 3.5m telescope and Minimosaic camera. For two of the galaxies, we combined the WIYN imaging with previously published data from the $\textit{Hubble Space Telescope}$ and the Keck Observatory to help characterize the GC distribution in the central few kiloparsecs. We determine the radial distribution (surface density of GCs versus projected radius) of each galaxy's GC system and use it to calculate the total number of GCs ($N_{GC}$). We find $N_{GC}$ = 490 ± 30, 210 ± 40, 175 ± 15, and 75 ± 10 for NGC1023, NGC1055, NGC7332, and NGC7339, respectively. We also calculate the GC specific frequency (N GC normalized by host galaxy luminosity or mass) and find values typical of those of the other spiral and E/S0 galaxies in the survey. The two lenticular galaxies have sufficient numbers of GC candidates for us to perform statistical tests for bimodality in the GC color distributions. We find evidence at a high confidence level (>95%) for two populations in the $B - R$ distribution of the GC system of NGC1023. We find weaker evidence for bimodality (>81% confidence) in the GC color distribution of NGC7332. Finally, we identify eight GC candidates that may be associated with the Magellanic dwarf galaxy NGC1023A, which is a satellite of NGC1023.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T19:34:00Z
No. of bitstreams: 1
1538-3881_144_4_103.pdf: 1654139 bytes, checksum: 9b6ccf37fef758186320b7096e8cadd9 (MD5)
Made available in DSpace on 2014-11-03T19:34:00Z (GMT). No. of bitstreams: 1
1538-3881_144_4_103.pdf: 1654139 bytes, checksum: 9b6ccf37fef758186320b7096e8cadd9 (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-6256/144/4/103
© 2012 The American Astronomical Society
galaxies: dwarf
galaxies: elliptical and lenticular, cD
galaxies: formation
galaxies: individual (NGC 7332, NGC 1055, NGC 1023, NGC 1023A, NGC 7339)
galaxies: spiral
galaxies: star clusters: general
Globular cluster systems of spiral and S0 galaxies: Results from WIYN imaging of NGC1023, NGC1055, NGC7332, and NGC7339
Article
true
ORIGINAL
1538-3881_144_4_103.pdf
1538-3881_144_4_103.pdf
application/pdf
1654139
https://scholarworks.iu.edu/dspace/bitstream/2022/19107/1/1538-3881_144_4_103.pdf
9b6ccf37fef758186320b7096e8cadd9
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19107/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
williams_john_license_2012.txt
williams_john_license_2012.txt
text/plain
4419
https://scholarworks.iu.edu/dspace/bitstream/2022/19107/3/williams_john_license_2012.txt
6ec64e44613167e5f92760fb0132622d
MD5
3
TEXT
1538-3881_144_4_103.pdf.txt
1538-3881_144_4_103.pdf.txt
Extracted text
text/plain
99551
https://scholarworks.iu.edu/dspace/bitstream/2022/19107/4/1538-3881_144_4_103.pdf.txt
fbebcd69af23fff4a7dab91c16901ebe
MD5
4
THUMBNAIL
1538-3881_144_4_103.pdf.jpg
1538-3881_144_4_103.pdf.jpg
IM Thumbnail
image/jpeg
2457
https://scholarworks.iu.edu/dspace/bitstream/2022/19107/5/1538-3881_144_4_103.pdf.jpg
db1d5189ca4082fd73e8d613fc3821d0
MD5
5
2022/19107
oai:scholarworks.iu.edu:2022/19107
2021-10-18 10:14:58.434
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/191092021-10-18T14:15:07Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Cheung, E.
Faber, S.M.
Koo, D.C.
Dutton, A.A.
Simard, L.
McGrath, E.J.
Huang, J.-S.
Bell, E.F.
Dekel, A.
Fang, J.J.
Salim, S.
Barro, G.
Bundy, K.
Coil, A.L.
Cooper, M.C.
Conselice, C.J.
Davis, M.
Domínguez, A.
Kassin, S.A.
Kocevski, D.D.
Koekemoer, A.M.
Lin, L.
Lotz, J.M.
Newman, J.a.
Phillips, A.C.
Rosario, D.J.
Weiner, B.J.
Willmer, C.N.A.
2014-11-03T19:58:37Z
2014-11-03T19:58:37Z
2012
Cheung, E., Faber, S. M., Koo, D. C., Dutton, A. A., Simard, L., McGrath, E. J., . . . Willmer, C. N. A. (2012). The dependence of quenching upon the inner structure of galaxies at 0.5 ≤ $z$ < 0.8 in the DEEP2/AEGIS survey. Astrophysical Journal, 760(2), 131. http://dx.doi.org/10.1088/0004-637X/760/2/131
http://hdl.handle.net/2022/19109
The shutdown of star formation in galaxies is generally termed "quenching." Quenching may occur through a variety of processes, e.g., active galactic nucleus (AGN) feedback, stellar feedback, or the shock heating of gas in the dark matter halo. However, which mechanism(s) is, in fact, responsible for quenching is still in question. This paper addresses quenching by searching for traces of possible quenching processes through their effects on galaxy structural parameters such as stellar mass ($M_{\ast }$), $M_{\ast }/r_{e}$, surface stellar mass density ($\sim M_{\ast }/r^{2}_{e}$), and Sérsic index ($n$). We analyze the rest-frame $U - B$ color correlations versus these structural parameters using a sample of galaxies in the redshift range $0.5 \lesssim z < 0.8$ from the DEEP2/AEGIS survey. In addition to global radii, stellar masses, and Sérsic parameters, we also use "bulge" and "disk" photometric measurements from GIM2D fits to $\textit{HST/ACS V}$ and $I$ images. We assess the tightness of the color relationships by measuring their "overlap regions," defined as the area in color-parameter space in which red and blue galaxies overlap; the parameter that minimizes these overlap regions is considered to be the most effective color discriminator. We find that Sérsic index ($n$) has the smallest overlap region among all tested parameters and resembles a step function with a threshold value of $n$ = 2.3. There exists, however, a significant population of outliers with blue colors yet high n values that seem to contradict this behavior; they make up $\approx$ 40% of $n$ > 2.3 galaxies. We hypothesize that their Sérsic values may be distorted by bursts of star formation, AGNs, and/or poor fits, leading us to consider central surface stellar mass density, $\sum^{\ast }_{1 \:\text{kpc}}$, as an alternative to Sérsic index. Not only does $\sum^{\ast }_{1 \:\text{kpc}}$ correct the outliers, but it also forms a tight relationship with color, suggesting that the $\textit{innermost structure of galaxies is most physically linked with quenching}$. Furthermore, at $z \sim 0.65$, the majority of the blue cloud galaxies cannot simply fade onto the red sequence since their GIM2D bulge masses are only half as large on average as the bulge masses of similar red sequence galaxies, thus demonstrating that stellar mass must absolutely increase at the centers of galaxies as they quench. We discuss a two-stage model for quenching in which galaxy star formation rates are controlled by their dark halos while they are still in the blue cloud and a second quenching process sets in later, associated with the central stellar mass buildup. The mass buildup is naturally explained by any non-axisymmetric features in the potential, such as those induced by mergers and/or disk instabilities. However, the identity of the second quenching agent is still unknown. We have placed our data catalog online
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T19:58:37Z
No. of bitstreams: 1
0004-637X_760_2_131.pdf: 4530651 bytes, checksum: 5653c9990c94b408763801328b69304d (MD5)
Made available in DSpace on 2014-11-03T19:58:37Z (GMT). No. of bitstreams: 1
0004-637X_760_2_131.pdf: 4530651 bytes, checksum: 5653c9990c94b408763801328b69304d (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/760/2/131
© 2012 The American Astronomical Society
galaxies: bulges
galaxies: evolution
galaxies: formation
galaxies: fundamental parameters
galaxies: structure
The dependence of quenching upon the inner structure of galaxies at 0.5 ≤ $z$ < 0.8 in the DEEP2/AEGIS survey
Article
false
ORIGINAL
0004-637X_760_2_131.pdf
0004-637X_760_2_131.pdf
application/pdf
4530651
https://scholarworks.iu.edu/dspace/bitstream/2022/19109/1/0004-637X_760_2_131.pdf
5653c9990c94b408763801328b69304d
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19109/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19109/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_760_2_131.pdf.txt
0004-637X_760_2_131.pdf.txt
Extracted text
text/plain
154178
https://scholarworks.iu.edu/dspace/bitstream/2022/19109/4/0004-637X_760_2_131.pdf.txt
77b5baba21115ff1100a0403fde0c2a7
MD5
4
THUMBNAIL
0004-637X_760_2_131.pdf.jpg
0004-637X_760_2_131.pdf.jpg
IM Thumbnail
image/jpeg
1884
https://scholarworks.iu.edu/dspace/bitstream/2022/19109/5/0004-637X_760_2_131.pdf.jpg
1e0fc0153c7ff117f755b32fc5d5a178
MD5
5
2022/19109
oai:scholarworks.iu.edu:2022/19109
2021-10-18 10:15:07.088
IUScholarWorks
iusw@indiana.edu
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
oai:scholarworks.iu.edu:2022/191102021-10-18T14:14:04Zcom_2022_12958com_2022_19675com_2022_19673col_2022_12959
Salim, S.
Fang, J.J.
Rich, R.M.
Faber, S.M.
Thilker, D.A.
2014-11-03T20:08:10Z
2014-11-03T20:08:10Z
2012
Salim, S., Fang, J. J., Rich, R. M., Faber, S. M., & Thilker, D. A. (2012). Galaxy-scale star formation on the red sequence: The continued growth of S0s and the quiescence of ellipticals. Astrophysical Journal, 755(2), 105. http://dx.doi.org/10.1088/0004-637X/755/2/105
http://hdl.handle.net/2022/19110
This paper examines star formation (SF) in relatively massive, primarily early-type galaxies (ETGs) at $z \sim 0.1$. A sample is drawn from bulge-dominated Galaxy Evolution Explorer/Sloan Digital Sky Survey (GALEX/SDSS) galaxies on the optical red sequence with strong UV excess and yet quiescent SDSS spectra. High-resolution far-UV imaging of 27 such ETGs using Hubble Space Telescope Advanced Camera for Surveys/Solar Blind Channel (ACS/SBC) reveals structured UV morphology in 93% of the sample, consistent with low-level ongoing SF ($\sim0.5 M_{\odot} yr^{–1}$). In 3/4 of the sample the SF is extended on galaxy scales (25-75 kpc), while the rest contains smaller (5-15 kpc) SF patches in the vicinity of an ETG—presumably gas-rich satellites being disrupted. Optical imaging reveals that all ETGs with galaxy-scale SF in our sample have old stellar disks (mostly S0 type). None is classified as a true elliptical. In our sample, galaxy-scale SF takes the form of UV rings of varying sizes and morphologies. For the majority of such objects we conclude that the gas needed to fuel current SF has been accreted from the intergalactic medium, probably in a prolonged, quasi-static manner, leading in some cases to additional disk buildup. The remaining ETGs with galaxy-scale SF have UV and optical morphologies consistent with minor merger-driven SF or with the final stages of SF in fading spirals. Our analysis excludes that all recent SF on the red sequence resulted from gas-rich mergers. We find further evidence that galaxy-scale SF is almost exclusively an S0 phenomenon ($\sim$20% S0s have SF) by examining the overall optically red SDSS ETGs. Conclusion is that significant number of field S0s maintain or resume low-level SF because the preventive feedback is not in place or is intermittent. True ellipticals, on the other hand, stay entirely quiescent even in the field.
Submitted by Yumiko Siewenie (ysieweni@indiana.edu) on 2014-11-03T20:08:10Z
No. of bitstreams: 1
0004-637X_755_2_105.pdf: 6921091 bytes, checksum: 627a0c3520ffd4b24c200ee41db1c0fd (MD5)
Made available in DSpace on 2014-11-03T20:08:10Z (GMT). No. of bitstreams: 1
0004-637X_755_2_105.pdf: 6921091 bytes, checksum: 627a0c3520ffd4b24c200ee41db1c0fd (MD5)
Previous issue date: 2012
en_US
The American Astronomical Society
https://doi.org/10.1088/0004-637X/755/2/105
© 2012 The American Astronomical Society
galaxies: evolution
ultraviolet: galaxies
galaxies: elliptical and lenticular, cD
Galaxy-scale star formation on the red sequence: The continued growth of S0s and the quiescence of ellipticals
Article
true
ORIGINAL
0004-637X_755_2_105.pdf
0004-637X_755_2_105.pdf
application/pdf
6921091
https://scholarworks.iu.edu/dspace/bitstream/2022/19110/1/0004-637X_755_2_105.pdf
627a0c3520ffd4b24c200ee41db1c0fd
MD5
1
LICENSE
license.txt
license.txt
text/plain
2012
https://scholarworks.iu.edu/dspace/bitstream/2022/19110/2/license.txt
2d12280d99d4502d180cd616e4c6d855
MD5
2
salim_samir_license_2012.txt
salim_samir_license_2012.txt
text/plain
9621
https://scholarworks.iu.edu/dspace/bitstream/2022/19110/3/salim_samir_license_2012.txt
9e525ec6cab57a0a6669a7186012dea3
MD5
3
TEXT
0004-637X_755_2_105.pdf.txt
0004-637X_755_2_105.pdf.txt
Extracted text
text/plain
158684
https://scholarworks.iu.edu/dspace/bitstream/2022/19110/4/0004-637X_755_2_105.pdf.txt
0f714ebbb471e7b7148968c65e8ac599
MD5
4
THUMBNAIL
0004-637X_755_2_105.pdf.jpg
0004-637X_755_2_105.pdf.jpg
IM Thumbnail
image/jpeg
3650
https://scholarworks.iu.edu/dspace/bitstream/2022/19110/5/0004-637X_755_2_105.pdf.jpg
d7a22edd28b9d2657a01759f044aa9a3
MD5
5
2022/19110
oai:scholarworks.iu.edu:2022/19110
2021-10-18 10:14:04.397
IUScholarWorks
iusw@indiana.edu
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