HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m

S. J. Oliver; L. Wang; A. J. Smith; B. Altieri; A. Amblard; V. Arumugam; R. Auld; H. Aussel; T. Babbedge; A. Blain; J. Bock; A. Boselli; V. Buat; D. Burgarella; N. Castro-Rodríguez; A. Cava; P. Chanial; D. L. Clements; A. Conley; L. Conversi; A. Cooray; C. D. Dowell; E. Dwek; S. Eales; D. Elbaz; M. Fox; A. Franceschini; W. Gear; J. Glenn; M. Griffin; M. Halpern; E. Hatziminaoglou; E. Ibar; K. Isaak; R. J. Ivison; G. Lagache; L. Levenson; N. Lu; S. Madden; B. Maffei; G. Mainetti; L. Marchetti; K. Mitchell-Wynne; A. M.J. Mortier; H. T. Nguyen; B. O'Halloran; A. Omont; M. J. Page; P. Panuzzo; A. Papageorgiou; C. P. Pearson; I. Pérez-Fournon; M. Pohlen; J. I. Rawlings; G. Raymond; D. Rigopoulou; D. Rizzo; I. G. Roseboom; M. Rowan-Robinson; M. Sánchez Portal; R. Savage; B. Schulz; D. Scott; N. Seymour; D. L. Shupe; J. A. Stevens; M. Symeonidis; M. Trichas; K. E. Tugwell; M. Vaccari; E. Valiante; I. Valtchanov; J. D. Vieira; L. Vigroux; R. Ward; G. Wright; C. K. Xu; M. Zemcov

doi:10.1051/0004-6361/201014697

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m

S. J. Oliver
, L. Wang
, A. J. Smith
, B. Altieri
, A. Amblard
, V. Arumugam
, R. Auld
, H. Aussel
, T. Babbedge
, A. Blain
, J. Bock
, A. Boselli
, V. Buat
, D. Burgarella
, N. Castro-Rodríguez
, A. Cava
, P. Chanial
, D. L. Clements
, A. Conley
, L. Conversi

A. Cooray, C. D. Dowell, E. Dwek, S. Eales, D. Elbaz, M. Fox, A. Franceschini, W. Gear, J. Glenn, M. Griffin, M. Halpern, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, L. Marchetti, K. Mitchell-Wynne, A. M.J. Mortier, H. T. Nguyen, B. O'Halloran, A. Omont, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, J. I. Rawlings, G. Raymond, D. Rigopoulou, D. Rizzo, I. G. Roseboom, M. Rowan-Robinson, M. Sánchez Portal, R. Savage, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, J. A. Stevens, M. Symeonidis, M. Trichas, K. E. Tugwell, M. Vaccari, E. Valiante, I. Valtchanov, J. D. Vieira, L. Vigroux, R. Ward, G. Wright, C. K. Xu, M. Zemcov

University of Sussex
European Space Astronomy Centre
University of California, Irvine
University of Edinburgh, Institute for Astronomy
Cardiff University
Université Paris Diderot
Imperial College London
California Institute of Technology
Jet Propulsion Laboratory
Laboratoire d'Astrophysique de Marseille
GTC Project
Universidad de la Laguna
University of Colorado Boulder
NASA Goddard Space Flight Center
University of Padova
University of British Columbia
ESO
Royal Observatory
Institut d'Astrophysique Spatiale
California Institute of Technology
University of Manchester
UPMC Univ. Paris 06
University College London
Rutherford Appleton Laboratory
University of Lethbridge
University of Oxford
University of Warwick
University of Hertfordshire

Research output: Contribution to a Journal (Peer & Non Peer) › Article › peer-review

212 Citations (Scopus)

Abstract

Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.

Original language	English
Article number	L21
Journal	Astronomy and Astrophysics
Volume	518
Issue number	7-8
DOIs	https://doi.org/10.1051/0004-6361/201014697
Publication status	Published - 16 Jul 2010
Externally published	Yes

Keywords

Galaxies: evolution
Submillimeter: galaxies
Surveys

Access to Document

10.1051/0004-6361/201014697

Cite this

Oliver, S. J., Wang, L., Smith, A. J., Altieri, B., Amblard, A., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., ... Zemcov, M. (2010). HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m. Astronomy and Astrophysics, 518(7-8), Article L21. https://doi.org/10.1051/0004-6361/201014697

@article{0d5a57d50f394c2abcd5d7dcf0b9d528,

title = "HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m",

abstract = "Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to \textasciitilde{}20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved \textasciitilde{}15\% of the infrared extra-galactic background at the wavelength near where it peaks.",

keywords = "Galaxies: evolution, Submillimeter: galaxies, Surveys",

author = "Oliver, \{S. J.\} and L. Wang and Smith, \{A. J.\} and B. Altieri and A. Amblard and V. Arumugam and R. Auld and H. Aussel and T. Babbedge and A. Blain and J. Bock and A. Boselli and V. Buat and D. Burgarella and N. Castro-Rodr{\'i}guez and A. Cava and P. Chanial and Clements, \{D. L.\} and A. Conley and L. Conversi and A. Cooray and Dowell, \{C. D.\} and E. Dwek and S. Eales and D. Elbaz and M. Fox and A. Franceschini and W. Gear and J. Glenn and M. Griffin and M. Halpern and E. Hatziminaoglou and E. Ibar and K. Isaak and Ivison, \{R. J.\} and G. Lagache and L. Levenson and N. Lu and S. Madden and B. Maffei and G. Mainetti and L. Marchetti and K. Mitchell-Wynne and Mortier, \{A. M.J.\} and Nguyen, \{H. T.\} and B. O'Halloran and A. Omont and Page, \{M. J.\} and P. Panuzzo and A. Papageorgiou and Pearson, \{C. P.\} and I. P{\'e}rez-Fournon and M. Pohlen and Rawlings, \{J. I.\} and G. Raymond and D. Rigopoulou and D. Rizzo and Roseboom, \{I. G.\} and M. Rowan-Robinson and \{S{\'a}nchez Portal\}, M. and R. Savage and B. Schulz and D. Scott and N. Seymour and Shupe, \{D. L.\} and Stevens, \{J. A.\} and M. Symeonidis and M. Trichas and Tugwell, \{K. E.\} and M. Vaccari and E. Valiante and I. Valtchanov and Vieira, \{J. D.\} and L. Vigroux and R. Ward and G. Wright and Xu, \{C. K.\} and M. Zemcov",

year = "2010",

month = jul,

day = "16",

doi = "10.1051/0004-6361/201014697",

language = "English",

volume = "518",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "7-8",

}

Oliver, SJ, Wang, L, Smith, AJ, Altieri, B, Amblard, A, Arumugam, V, Auld, R, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodríguez, N, Cava, A, Chanial, P, Clements, DL, Conley, A, Conversi, L, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Elbaz, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Mitchell-Wynne, K, Mortier, AMJ, Nguyen, HT, O'Halloran, B, Omont, A, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Pérez-Fournon, I, Pohlen, M, Rawlings, JI, Raymond, G, Rigopoulou, D, Rizzo, D, Roseboom, IG, Rowan-Robinson, M, Sánchez Portal, M, Savage, R, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vaccari, M, Valiante, E, Valtchanov, I, Vieira, JD, Vigroux, L, Ward, R, Wright, G, Xu, CK & Zemcov, M 2010, 'HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m', Astronomy and Astrophysics, vol. 518, no. 7-8, L21. https://doi.org/10.1051/0004-6361/201014697

TY - JOUR

T1 - HerMES

T2 - SPIRE galaxy number counts at 250, 350, and 500 μ m

AU - Oliver, S. J.

AU - Wang, L.

AU - Smith, A. J.

AU - Altieri, B.

AU - Amblard, A.

AU - Arumugam, V.

AU - Auld, R.

AU - Aussel, H.

AU - Babbedge, T.

AU - Blain, A.

AU - Bock, J.

AU - Boselli, A.

AU - Buat, V.

AU - Burgarella, D.

AU - Castro-Rodríguez, N.

AU - Cava, A.

AU - Chanial, P.

AU - Clements, D. L.

AU - Conley, A.

AU - Conversi, L.

AU - Cooray, A.

AU - Dowell, C. D.

AU - Dwek, E.

AU - Eales, S.

AU - Elbaz, D.

AU - Fox, M.

AU - Franceschini, A.

AU - Gear, W.

AU - Glenn, J.

AU - Griffin, M.

AU - Halpern, M.

AU - Hatziminaoglou, E.

AU - Ibar, E.

AU - Isaak, K.

AU - Ivison, R. J.

AU - Lagache, G.

AU - Levenson, L.

AU - Lu, N.

AU - Madden, S.

AU - Maffei, B.

AU - Mainetti, G.

AU - Marchetti, L.

AU - Mitchell-Wynne, K.

AU - Mortier, A. M.J.

AU - Nguyen, H. T.

AU - O'Halloran, B.

AU - Omont, A.

AU - Page, M. J.

AU - Panuzzo, P.

AU - Papageorgiou, A.

AU - Pearson, C. P.

AU - Pérez-Fournon, I.

AU - Pohlen, M.

AU - Rawlings, J. I.

AU - Raymond, G.

AU - Rigopoulou, D.

AU - Rizzo, D.

AU - Roseboom, I. G.

AU - Rowan-Robinson, M.

AU - Sánchez Portal, M.

AU - Savage, R.

AU - Schulz, B.

AU - Scott, D.

AU - Seymour, N.

AU - Shupe, D. L.

AU - Stevens, J. A.

AU - Symeonidis, M.

AU - Trichas, M.

AU - Tugwell, K. E.

AU - Vaccari, M.

AU - Valiante, E.

AU - Valtchanov, I.

AU - Vieira, J. D.

AU - Vigroux, L.

AU - Ward, R.

AU - Wright, G.

AU - Xu, C. K.

AU - Zemcov, M.

PY - 2010/7/16

Y1 - 2010/7/16

N2 - Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.

AB - Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.

KW - Galaxies: evolution

KW - Submillimeter: galaxies

KW - Surveys

UR - https://www.scopus.com/pages/publications/77957855162

U2 - 10.1051/0004-6361/201014697

DO - 10.1051/0004-6361/201014697

M3 - Article

AN - SCOPUS:77957855162

SN - 0004-6361

VL - 518

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 7-8

M1 - L21

ER -

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m

Abstract

Keywords

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