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A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions

Identificadores del recurso

The Astrophysical Journal 912(2): 161(2021)

0004-637X

https://iopscience.iop.org/article/10.3847/1538-4357/abec50

http://hdl.handle.net/20.500.12666/628

10.3847/1538-4357/abec50

1538-4357

http://dx.doi.org/10.13039/501100001809

http://dx.doi.org/10.13039/501100002367

http://dx.doi.org/10.13039/501100001732

http://dx.doi.org/10.13039/501100000271

Procedencia

(Digital.INTA - Repositorio institucional del INTA)

Ficha

Título:: A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions
Tema:: Infrared galaxies; Luminous infrared galaxies; Sky surveys; Spectral energy distribution
Descripción:: We describe a complete, flux-density-limited sample of galaxies at redshift 0.8 < z < 1.3 selected at 16 μm. At the selection wavelength near 8 μm rest, the observed emission comes from both dust heated by intense star formation and active galactic nuclei (AGNs). Fitting the spectral energy distributions (SEDs) of the sample galaxies to local-galaxy templates reveals that more than half the galaxies have SEDs dominated by star formation. About one-sixth of the galaxy SEDs are dominated by an AGN, and nearly all of the rest of the SEDs are composite. Comparison with X-ray and far-infrared observations shows that combinations of luminosities at rest-frame 4.5 and 8 μm give good measures of both AGN luminosity and star formation rate. The sample galaxies mostly follow the established star-forming main sequence for z = 1 galaxies, but of the galaxies more than 0.5 dex above that main sequence, more than half have AGN-type SEDs. Similarly, the most luminous AGNs tend to have higher star formation rates than the main-sequence value. Galaxies with stellar masses >1011 M⊙ are unlikely to host an AGN. About 1% of the sample galaxies show an SED with dust emission typical of neither star formation nor an AGN.; This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by the Chinese National Nature Science Foundation grant No. 10878003. This work was supported in part by the National Key R&D Program of China via grant No. 2017YFA0402703 and by NSFC grants 11433003, 11822303, 11773020, 11733002, 11933003, 11373034, 11803044, and 11673028. Additional support came from the Chinese Academy of Sciences (CAS) through a grant to the South America Center for Astronomy (CASSACA) in Santiago, Chile. G.M. acknowledges the Villum Fonden research grant 13160 Gas to stars, stars to dust: tracing star formation across cosmic time and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under grant No. 140. D.R. acknowledges support from STFC through grant No. ST.S000488.1.; Peerreview
Idioma:: English
Autor/Productor:: Huang, J. S.; Dai, Y. S.; Willner, S. P.; Faber, S. M.; Cheng, C.; Xu, H.; Yan, H.; Wu, S.; Shao, X.; Hao, C.; Xia, X.; Rigopoulou, D.; Pereira Santaella, M.; Magdis, G.; Cortzen, I.; Fazio, G. G.; Assmann, P.; Fan, L.; Musin, M.; Zang, Z.; Xu, K. C.; He, C.; Jin, G.; Esamdin, A.
Editor:: IOP Science Publishing
Otros colaboradores/productores:: Huang, J. S. [0000-0001-6511-8745]; Dai, Y. S. [0000-0002-7928-416X]; Willner, S. P. [0000-0002-9895-5758]; Faber, S. M. [0000-0003-4996-214X]; Cheng, C. [0000-0003-0202-0534]; Yan, H. [0000-0001-7592-7714]; Rigopoulou, D. [0000-0001-6854-7545]; Pereira Santaella, M. [0000-0002-4005-9619]; Magdis, G. [0000-0002-4872-2294]; Cortzen, I. [0000-0001-9197-7623]; Fazio, G. G. [0000-0002-0670-0708]; Fan, L. [0000-0003-4200-4432]; Jin, G. [0000-0003-3087-318X]; Esamdin, A. [0000-0003-1845-4900]; National Natural Science Foundation of China (NSFC); Chinese Academy of Sciences (CAS); Danish National Research Foundation (DNRF); Science and Technology Facilities Council (STFC); South America Center for Astronomy (CASSACA)
Derechos:: Attribution-NonCommercial-NoDerivatives 4.0 International; Published 2021 May 28 • © 2021. The American Astronomical Society. All rights reserved.; https://creativecommons.org/licenses/by-nc-nd/4.0/; info:eu-repo/semantics/openAccess
Fecha:: 2022-02-16T07:38:47Z; 2021-05-28
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Formato:: application/pdf

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1. < dc:title > A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions </ dc:title >
2. < dc:creator > Huang, J. S. </ dc:creator >
3. < dc:creator > Dai, Y. S. </ dc:creator >
4. < dc:creator > Willner, S. P. </ dc:creator >
5. < dc:creator > Faber, S. M. </ dc:creator >
6. < dc:creator > Cheng, C. </ dc:creator >
7. < dc:creator > Xu, H. </ dc:creator >
8. < dc:creator > Yan, H. </ dc:creator >
9. < dc:creator > Wu, S. </ dc:creator >
10. < dc:creator > Shao, X. </ dc:creator >
11. < dc:creator > Hao, C. </ dc:creator >
12. < dc:creator > Xia, X. </ dc:creator >
13. < dc:creator > Rigopoulou, D. </ dc:creator >
14. < dc:creator > Pereira Santaella, M. </ dc:creator >
15. < dc:creator > Magdis, G. </ dc:creator >
16. < dc:creator > Cortzen, I. </ dc:creator >
17. < dc:creator > Fazio, G. G. </ dc:creator >
18. < dc:creator > Assmann, P. </ dc:creator >
19. < dc:creator > Fan, L. </ dc:creator >
20. < dc:creator > Musin, M. </ dc:creator >
21. < dc:creator > Zang, Z. </ dc:creator >
22. < dc:creator > Xu, K. C. </ dc:creator >
23. < dc:creator > He, C. </ dc:creator >
24. < dc:creator > Jin, G. </ dc:creator >
25. < dc:creator > Esamdin, A. </ dc:creator >
26. < dc:contributor > Huang, J. S. [0000-0001-6511-8745] </ dc:contributor >
27. < dc:contributor > Dai, Y. S. [0000-0002-7928-416X] </ dc:contributor >
28. < dc:contributor > Willner, S. P. [0000-0002-9895-5758] </ dc:contributor >
29. < dc:contributor > Faber, S. M. [0000-0003-4996-214X] </ dc:contributor >
30. < dc:contributor > Cheng, C. [0000-0003-0202-0534] </ dc:contributor >
31. < dc:contributor > Yan, H. [0000-0001-7592-7714] </ dc:contributor >
32. < dc:contributor > Rigopoulou, D. [0000-0001-6854-7545] </ dc:contributor >
33. < dc:contributor > Pereira Santaella, M. [0000-0002-4005-9619] </ dc:contributor >
34. < dc:contributor > Magdis, G. [0000-0002-4872-2294] </ dc:contributor >
35. < dc:contributor > Cortzen, I. [0000-0001-9197-7623] </ dc:contributor >
36. < dc:contributor > Fazio, G. G. [0000-0002-0670-0708] </ dc:contributor >
37. < dc:contributor > Fan, L. [0000-0003-4200-4432] </ dc:contributor >
38. < dc:contributor > Jin, G. [0000-0003-3087-318X] </ dc:contributor >
39. < dc:contributor > Esamdin, A. [0000-0003-1845-4900] </ dc:contributor >
40. < dc:contributor > National Natural Science Foundation of China (NSFC) </ dc:contributor >
41. < dc:contributor > Chinese Academy of Sciences (CAS) </ dc:contributor >
42. < dc:contributor > Danish National Research Foundation (DNRF) </ dc:contributor >
43. < dc:contributor > Science and Technology Facilities Council (STFC) </ dc:contributor >
44. < dc:contributor > South America Center for Astronomy (CASSACA) </ dc:contributor >
45. < dc:subject > Infrared galaxies </ dc:subject >
46. < dc:subject > Luminous infrared galaxies </ dc:subject >
47. < dc:subject > Sky surveys </ dc:subject >
48. < dc:subject > Spectral energy distribution </ dc:subject >
49. < dc:description > We describe a complete, flux-density-limited sample of galaxies at redshift 0.8 < z < 1.3 selected at 16 μm. At the selection wavelength near 8 μm rest, the observed emission comes from both dust heated by intense star formation and active galactic nuclei (AGNs). Fitting the spectral energy distributions (SEDs) of the sample galaxies to local-galaxy templates reveals that more than half the galaxies have SEDs dominated by star formation. About one-sixth of the galaxy SEDs are dominated by an AGN, and nearly all of the rest of the SEDs are composite. Comparison with X-ray and far-infrared observations shows that combinations of luminosities at rest-frame 4.5 and 8 μm give good measures of both AGN luminosity and star formation rate. The sample galaxies mostly follow the established star-forming main sequence for z = 1 galaxies, but of the galaxies more than 0.5 dex above that main sequence, more than half have AGN-type SEDs. Similarly, the most luminous AGNs tend to have higher star formation rates than the main-sequence value. Galaxies with stellar masses >1011 M⊙ are unlikely to host an AGN. About 1% of the sample galaxies show an SED with dust emission typical of neither star formation nor an AGN. </ dc:description >
50. < dc:description > This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by the Chinese National Nature Science Foundation grant No. 10878003. This work was supported in part by the National Key R&D Program of China via grant No. 2017YFA0402703 and by NSFC grants 11433003, 11822303, 11773020, 11733002, 11933003, 11373034, 11803044, and 11673028. Additional support came from the Chinese Academy of Sciences (CAS) through a grant to the South America Center for Astronomy (CASSACA) in Santiago, Chile. G.M. acknowledges the Villum Fonden research grant 13160 Gas to stars, stars to dust: tracing star formation across cosmic time and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under grant No. 140. D.R. acknowledges support from STFC through grant No. ST.S000488.1. </ dc:description >
51. < dc:description > Peerreview </ dc:description >
52. < dc:date > 2022-02-16T07:38:47Z </ dc:date >
53. < dc:date > 2022-02-16T07:38:47Z </ dc:date >
54. < dc:date > 2021-05-28 </ dc:date >
55. < dc:type > info:eu-repo/semantics/article </ dc:type >
56. < dc:type > info:eu-repo/semantics/publishedVersion </ dc:type >
57. < dc:type > http://purl.org/coar/resource_type/c_6501 </ dc:type >
58. < dc:identifier > The Astrophysical Journal 912(2): 161(2021) </ dc:identifier >
59. < dc:identifier > 0004-637X </ dc:identifier >
60. < dc:identifier > https://iopscience.iop.org/article/10.3847/1538-4357/abec50 </ dc:identifier >
61. < dc:identifier > http://hdl.handle.net/20.500.12666/628 </ dc:identifier >
62. < dc:identifier > 10.3847/1538-4357/abec50 </ dc:identifier >
63. < dc:identifier > 1538-4357 </ dc:identifier >
64. < dc:identifier > http://dx.doi.org/10.13039/501100001809 </ dc:identifier >
65. < dc:identifier > http://dx.doi.org/10.13039/501100002367 </ dc:identifier >
66. < dc:identifier > http://dx.doi.org/10.13039/501100001732 </ dc:identifier >
67. < dc:identifier > http://dx.doi.org/10.13039/501100000271 </ dc:identifier >
68. < dc:language > eng </ dc:language >
69. < dc:rights > Attribution-NonCommercial-NoDerivatives 4.0 International </ dc:rights >
70. < dc:rights > Published 2021 May 28 • © 2021. The American Astronomical Society. All rights reserved. </ dc:rights >
71. < dc:rights > https://creativecommons.org/licenses/by-nc-nd/4.0/ </ dc:rights >
72. < dc:rights > info:eu-repo/semantics/openAccess </ dc:rights >
73. < dc:format > application/pdf </ dc:format >
74. < dc:publisher > IOP Science Publishing </ dc:publisher >
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