Evolution of dust temperature of galaxies through cosmic time as seen by Herschel†

  1. H. S. Hwang1,*,
  2. D. Elbaz1,
  3. G. Magdis1,
  4. E. Daddi1,
  5. M. Symeonidis2,
  6. B. Altieri3,
  7. A. Amblard4,
  8. P. Andreani5,6,
  9. V. Arumugam7,
  10. R. Auld8,
  11. H. Aussel1,
  12. T. Babbedge9,
  13. S. Berta10,
  14. A. Blain11,
  15. J. Bock11,12,
  16. A. Bongiovanni13,14,
  17. A. Boselli15,
  18. V. Buat15,
  19. D. Burgarella15,
  20. N. Castro-Rodríguez13,14,
  21. A. Cava13,14,
  22. J. Cepa13,14,
  23. P. Chanial9,
  24. E. Chapin16,
  25. R.-R. Chary17,
  26. A. Cimatti18,
  27. D. L. Clements9,
  28. A. Conley19,
  29. L. Conversi3,
  30. A. Cooray4,11,
  31. H. Dannerbauer1,
  32. M. Dickinson20,
  33. H. Dominguez21,
  34. C. D. Dowell11,12,
  35. J. S. Dunlop7,
  36. E. Dwek22,
  37. S. Eales8,
  38. D. Farrah23,
  39. N. Förster Schreiber10,
  40. M. Fox9,
  41. A. Franceschini24,
  42. W. Gear8,
  43. R. Genzel10,
  44. J. Glenn19,
  45. M. Griffin8,
  46. C. Gruppioni25,
  47. M. Halpern16,
  48. E. Hatziminaoglou5,
  49. E. Ibar26,
  50. K. Isaak8,
  51. R. J. Ivison7,26,
  52. W.-S. Jeong27,
  53. G. Lagache28,
  54. D. Le Borgne29,
  55. E. Le Floc’h1,
  56. H. M. Lee30,
  57. J. C. Lee30,
  58. M. G. Lee30,
  59. L. Levenson11,12,
  60. N. Lu11,31,
  61. D. Lutz10,
  62. S. Madden1,
  63. B. Maffei32,
  64. B. Magnelli10,
  65. G. Mainetti24,
  66. R. Maiolino21,
  67. L. Marchetti24,
  68. A. M. J. Mortier9,
  69. H. T. Nguyen11,12,
  70. R. Nordon10,
  71. B. O’Halloran9,
  72. K. Okumura1,
  73. S. J. Oliver23,
  74. A. Omont29,
  75. M. J. Page2,
  76. P. Panuzzo1,
  77. A. Papageorgiou8,
  78. C. P. Pearson33,34,
  79. I. Pérez-Fournon13,14,
  80. A. M. Pérez García13,14,
  81. A. Poglitsch10,
  82. M. Pohlen8,
  83. P. Popesso10,
  84. F. Pozzi25,
  85. J. I. Rawlings2,
  86. D. Rigopoulou33,35,
  87. L. Riguccini1,
  88. D. Rizzo9,
  89. G. Rodighiero24,
  90. I. G. Roseboom23,
  91. M. Rowan-Robinson9,
  92. A. Saintonge10,
  93. M. Sánchez Portal3,
  94. P. Santini21,
  95. M. Sauvage1,
  96. B. Schulz11,31,
  97. D. Scott16,
  98. N. Seymour2,
  99. L. Shao10,
  100. D. L. Shupe11,31,
  101. A. J. Smith23,
  102. J. A. Stevens36,
  103. E. Sturm10,
  104. L. Tacconi10,
  105. M. Trichas9,
  106. K. E. Tugwell2,
  107. M. Vaccari24,
  108. I. Valtchanov3,
  109. J. D. Vieira11,
  110. L. Vigroux29,
  111. L. Wang23,
  112. R. Ward23,
  113. G. Wright26,
  114. C. K. Xu11,31,
  115. M. Zemcov11,12

Article first published online: 25 OCT 2010

DOI: 10.1111/j.1365-2966.2010.17645.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 409, Issue 1, pages 75–82, November 2010

Additional Information

How to Cite

Hwang, H. S., Elbaz, D., Magdis, G., Daddi, E., Symeonidis, M., Altieri, B., Amblard, A., Andreani, P., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Cepa, J., Chanial, P., Chapin, E., Chary, R.-R., Cimatti, A., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dannerbauer, H., Dickinson, M., Dominguez, H., Dowell, C. D., Dunlop, J. S., Dwek, E., Eales, S., Farrah, D., Schreiber, N. F., Fox, M., Franceschini, A., Gear, W., Genzel, R., Glenn, J., Griffin, M., Gruppioni, C., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Jeong, W.-S., Lagache, G., Le Borgne, D., Le Floc’h, E., Lee, H. M., Lee, J. C., Lee, M. G., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magnelli, B., Mainetti, G., Maiolino, R., Marchetti, L., Mortier, A. M. J., Nguyen, H. T., Nordon, R., O’Halloran, B., Okumura, K., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., García, A. M. P., Poglitsch, A., Pohlen, M., Popesso, P., Pozzi, F., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Saintonge, A., Portal, M. S., Santini, P., Sauvage, M., Schulz, B., Scott, D., Seymour, N., Shao, L., Shupe, D. L., Smith, A. J., Stevens, J. A., Sturm, E., Tacconi, L., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K. and Zemcov, M. (2010), Evolution of dust temperature of galaxies through cosmic time as seen by Herschel. Monthly Notices of the Royal Astronomical Society, 409: 75–82. doi: 10.1111/j.1365-2966.2010.17645.x

Author Information

  1. 1

    Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette, France

  2. 2

    Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT

  3. 3

    Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada 28691 Madrid, Spain

  4. 4

    Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA

  5. 5

    ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany

  6. 6

    INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy

  7. 7

    Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ

  8. 8

    Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA

  9. 9

    Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ

  10. 10

    Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741, Garching, Germany

  11. 11

    California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA

  12. 12

    Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA

  13. 13

    Instituto de Astrofísica de Canarias (IAC), E-38200 La Laguna, Tenerife, Spain

  14. 14

    Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Tenerife, Spain

  15. 15

    Laboratoire d’Astrophysique de Marseille, OAMP, Université Aix-marseille, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille cedex 13, France

  16. 16

    Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver BC V6T 1Z1, Canada

  17. 17

    Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA

  18. 18

    Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna, Italy

  19. 19

    Department of Astrophysical and Planetary Sciences, CASA 389-UCB, University of Colorado, Boulder, CO 80309, USA

  20. 20

    National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA

  21. 21

    INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy

  22. 22

    Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

  23. 23

    Astronomy Centre, Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH

  24. 24

    Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, 3, 35122 Padova, Italy

  25. 25

    INAF – Osservatorio Astronomico di Roma, via di Franscati 33, 00040 Monte Porzio Catone, Italy

  26. 26

    UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ

  27. 27

    Korea Astronomy & Space Science Institute, Deajeon 305-348, Korea

  28. 28

    Institut d’Astrophysique Spatiale (IAS), bâtiment 121, Université Paris-Sud 11 and CNRS (UMR 8617), 91405 Orsay, France

  29. 29

    Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis boulevard Arago, F-75014 Paris, France

  30. 30

    Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea

  31. 31

    Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, CA 91125, USA

  32. 32

    School of Physics and Astronomy, The University of Manchester, Alan Turing Building, Oxford Road, Manchester M13 9PL

  33. 33

    Space Science & Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX

  34. 34

    Institute for Space Imaging Science, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada

  35. 35

    Astrophysics, Oxford University, Keble Road, Oxford OX1 3RH

  36. 36

    Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB

* E-mail: hoseong.hwang@cea.fr

  1. †

    Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Publication History

  1. Issue published online: 9 NOV 2010
  2. Article first published online: 25 OCT 2010
  3. Accepted 2010 September 3. Received 2010 July 26

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Keywords:

  • galaxies: evolution;
  • galaxies: formation;
  • galaxies: general;
  • galaxies: high-redshift;
  • galaxies: starburst;
  • infrared: galaxies

ABSTRACT

We study the dust properties of galaxies in the redshift range 0.1 ≲z≲ 2.8 observed by the Herschel Space Observatory in the field of the Great Observatories Origins Deep Survey-North as part of the PACS Extragalactic Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) key programmes. Infrared (IR) luminosity (LIR) and dust temperature (Tdust) of galaxies are derived from the spectral energy distribution fit of the far-IR (FIR) flux densities obtained with the PACS and SPIRE instruments onboard Herschel. As a reference sample, we also obtain IR luminosities and dust temperatures of local galaxies at z < 0.1 using AKARI and IRAS data in the field of the Sloan Digital Sky Survey. We compare the LIR–Tdust relation between the two samples and find that the median Tdust of Herschel-selected galaxies at z≳ 0.5 with LIR≳ 5 × 1010 L⊙ appears to be 2–5 K colder than that of AKARI-selected local galaxies with similar luminosities, and the dispersion in Tdust for high-z galaxies increases with LIR due to the existence of cold galaxies that are not seen among local galaxies. We show that this large dispersion of the LIR−Tdust relation can bridge the gap between local star-forming galaxies and high-z submillimetre galaxies (SMGs). We also find that three SMGs with very low Tdust (≲20 K) covered in this study have close neighbouring sources with similar 24-μm brightness, which could lead to an overestimation of FIR/(sub)millimetre fluxes of the SMGs.

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