HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

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

doi:10.1111/j.1365-2966.2010.17781.x

HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

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

Research output: Contribution to journal › Article › peer-review

Abstract

Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 μm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam-1, approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam. © 2010 The Authors. Journal compilation © 2010 RAS.

Original language	English
Pages (from-to)	109-121
Number of pages	12
Journal	Monthly Notices of the Royal Astronomical Society
Volume	409
Issue number	1
DOIs	https://doi.org/10.1111/j.1365-2966.2010.17781.x
Publication status	Published - Nov 2010

Keywords

Cosmology: observations
Submillimetre: diffuse background
Submillimetre: galaxies

Access to Document

10.1111/j.1365-2966.2010.17781.x

http://adsabs.harvard.edu/abs/2010MNRAS.409..109G

Cite this

Glenn, J., Conley, A., Béthermin, M., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodríguez, N., Cava, A., Chanial, P., Clements, D. L., Conversi, L., Cooray, A., Dowell, C. D., ... Zemcov, M. (2010). HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations. Monthly Notices of the Royal Astronomical Society, 409(1), 109-121. https://doi.org/10.1111/j.1365-2966.2010.17781.x

@article{51879b8c84cb4d1bb6e4db737b61f2fc,

title = "HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations",

abstract = "Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 μm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam-1, approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.",

keywords = "Cosmology: observations, Submillimetre: diffuse background, Submillimetre: galaxies",

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

note = "DOI: 10.1111/j.1365-2966.2010.17781.x; eprintid: arXiv:1009.5675",

year = "2010",

month = nov,

doi = "10.1111/j.1365-2966.2010.17781.x",

language = "English",

volume = "409",

pages = "109--121",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "1365-2966",

publisher = "Oxford University Press",

number = "1",

}

Glenn, J, Conley, A, Béthermin, M, Altieri, B, Amblard, A, Arumugam, V, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Buat, V, Castro-Rodríguez, N, Cava, A, Chanial, P, Clements, DL, Conversi, L, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Elbaz, D, Ellsworth-Bowers, TP, Fox, M, Franceschini, A, Gear, W, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Laurent, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Marsden, G, Nguyen, HT, O'Halloran, B, Oliver, SJ, Omont, A, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Pérez-Fournon, I, Pohlen, M, Rigopoulou, D, Rizzo, D, Roseboom, IG, Rowan-Robinson, M, Portal, MS, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vaccari, M, Valtchanov, I, Vieira, JD, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, CK & Zemcov, M 2010, 'HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations', Monthly Notices of the Royal Astronomical Society, vol. 409, no. 1, pp. 109-121. https://doi.org/10.1111/j.1365-2966.2010.17781.x

TY - JOUR

T1 - HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

AU - Glenn, J.

AU - Conley, A.

AU - Béthermin, M.

AU - Altieri, B.

AU - Amblard, A.

AU - Arumugam, V.

AU - Aussel, H.

AU - Babbedge, T.

AU - Blain, A.

AU - Bock, J.

AU - Boselli, A.

AU - Buat, V.

AU - Castro-Rodríguez, N.

AU - Cava, A.

AU - Chanial, P.

AU - Clements, D. L.

AU - Conversi, L.

AU - Cooray, A.

AU - Dowell, C. D.

AU - Dwek, E.

AU - Eales, S.

AU - Elbaz, D.

AU - Ellsworth-Bowers, T. P.

AU - Fox, M.

AU - Franceschini, A.

AU - Gear, W.

AU - Griffin, M.

AU - Halpern, M.

AU - Hatziminaoglou, E.

AU - Ibar, E.

AU - Isaak, K.

AU - Ivison, R. J.

AU - Lagache, G.

AU - Laurent, G.

AU - Levenson, L.

AU - Lu, N.

AU - Madden, S.

AU - Maffei, B.

AU - Mainetti, G.

AU - Marchetti, L.

AU - Marsden, G.

AU - Nguyen, H. T.

AU - O'Halloran, B.

AU - Oliver, S. J.

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 - Rigopoulou, D.

AU - Rizzo, D.

AU - Roseboom, I. G.

AU - Rowan-Robinson, M.

AU - Portal, M. Sánchez

AU - Schulz, B.

AU - Scott, Douglas

AU - Seymour, N.

AU - Shupe, D. L.

AU - Smith, A. J.

AU - Stevens, J. A.

AU - Symeonidis, M.

AU - Trichas, M.

AU - Tugwell, K. E.

AU - Vaccari, M.

AU - Valtchanov, I.

AU - Vieira, J. D.

AU - Vigroux, L.

AU - Wang, L.

AU - Ward, R.

AU - Wright, G.

AU - Xu, C. K.

AU - Zemcov, M.

N1 - DOI: 10.1111/j.1365-2966.2010.17781.x; eprintid: arXiv:1009.5675

PY - 2010/11

Y1 - 2010/11

N2 - Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 μm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam-1, approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam. © 2010 The Authors. Journal compilation © 2010 RAS.

AB - Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 μm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam-1, approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam. © 2010 The Authors. Journal compilation © 2010 RAS.

KW - Cosmology: observations

KW - Submillimetre: diffuse background

KW - Submillimetre: galaxies

U2 - 10.1111/j.1365-2966.2010.17781.x

DO - 10.1111/j.1365-2966.2010.17781.x

M3 - Article

SN - 1365-2966

VL - 409

SP - 109

EP - 121

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

HerMES: Deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

Abstract

Keywords

Access to Document

Fingerprint

Cite this