Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses

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

doi:10.1038/nature09771

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses

A. Amblard, A. Cooray, P. Serra, B. Altieri, V. Arumugam, H. Aussel, A. Blain, J. Bock, A. Boselli, V. Buat, N. Castro-Rodriguez, A. Cava, P. Chanial, E. Chapin, D. Clements, A. Conley, L. Conversi, C.D. Dowell, E. Dwek, S. EalesD. Elbaz, D. Farrah, A. Franceschini, W.K. Gear, J. Glenn, M. Griffin, M. Halpern, E. Hatziminaoglou, E. Ibar, K.G. Isaak, R.J. Ivison, A.A. Khostovan, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, L. Marchetti, G. Marsden, K. Mitchell-Wynne, H.T. Nguyen, B. O'Halloran, S. Oliver, A. Omont, M.J. Page, P. Panuzzo, A. Papageorgiou, C.P. Pearson, I. Perez-Fournon, M. Pohlen, N. Rangwala, I.G. Roseboom, M. Rowan-Robinson, M.S. Portal, B. Schulz, D. Scott, N. Seymour, D. Shupe, A.J. Smith, Jason Stevens, M. Symeonidis, M. Trichas, K.E. Tugwell, M. Vaccari, E. Valiante, I. Valtchanov, J. Vieira, L. Vigroux, L. Wang, R. Ward, G. Wright, C.K. Xu, M. Zemcov

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

90 Citations (Scopus)

39 Downloads (Pure)

Abstract

The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).

Original language	English
Pages (from-to)	510-512
Journal	Nature
Volume	470
Issue number	7335
DOIs	https://doi.org/10.1038/nature09771
Publication status	Published - 2011

Keywords

Herschel-spire instrument
star formation
number counts
Hermes
redshift
spitzer
atlas
bias

Access to Document

10.1038/nature09771

905126Accepted author manuscript, 1.11 MB

Cite this

Amblard, A., Cooray, A., Serra, P., Altieri, B., Arumugam, V., Aussel, H., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodriguez, N., Cava, A., Chanial, P., Chapin, E., Clements, D., Conley, A., Conversi, L., Dowell, C. D., Dwek, E., ... Zemcov, M. (2011). Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses. Nature, 470(7335), 510-512. https://doi.org/10.1038/nature09771

@article{884ad5bfdb0c4b19b01eaa5db9bb3974,

title = "Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses",

abstract = "The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).",

keywords = "Herschel-spire instrument, star formation, number counts, Hermes, redshift, spitzer, atlas, bias",

author = "A. Amblard and A. Cooray and P. Serra and B. Altieri and V. Arumugam and H. Aussel and A. Blain and J. Bock and A. Boselli and V. Buat and N. Castro-Rodriguez and A. Cava and P. Chanial and E. Chapin and D. Clements and A. Conley and L. Conversi and C.D. Dowell and E. Dwek and S. Eales and D. Elbaz and D. Farrah and A. Franceschini and W.K. Gear and J. Glenn and M. Griffin and M. Halpern and E. Hatziminaoglou and E. Ibar and K.G. Isaak and R.J. Ivison and A.A. Khostovan and G. Lagache and L. Levenson and N. Lu and S. Madden and B. Maffei and G. Mainetti and L. Marchetti and G. Marsden and K. Mitchell-Wynne and H.T. Nguyen and B. O'Halloran and S. Oliver and A. Omont and M.J. Page and P. Panuzzo and A. Papageorgiou and C.P. Pearson and I. Perez-Fournon and M. Pohlen and N. Rangwala and I.G. Roseboom and M. Rowan-Robinson and M.S. Portal and B. Schulz and D. Scott and N. Seymour and D. Shupe and A.J. Smith and Jason Stevens and M. Symeonidis and M. Trichas and K.E. Tugwell and M. Vaccari and E. Valiante and I. Valtchanov and J. Vieira and L. Vigroux and L. Wang and R. Ward and G. Wright and C.K. Xu and M. Zemcov",

note = "Original article can be found at: http://www.nature.com/ Copyright Nature Publishing Group",

year = "2011",

doi = "10.1038/nature09771",

language = "English",

volume = "470",

pages = "510--512",

journal = "Nature",

issn = "0028-0836",

publisher = "Nature Research",

number = "7335",

}

Amblard, A, Cooray, A, Serra, P, Altieri, B, Arumugam, V, Aussel, H, Blain, A, Bock, J, Boselli, A, Buat, V, Castro-Rodriguez, N, Cava, A, Chanial, P, Chapin, E, Clements, D, Conley, A, Conversi, L, Dowell, CD, Dwek, E, Eales, S, Elbaz, D, Farrah, D, Franceschini, A, Gear, WK, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, KG, Ivison, RJ, Khostovan, AA, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Marsden, G, Mitchell-Wynne, K, Nguyen, HT, O'Halloran, B, Oliver, S, Omont, A, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Perez-Fournon, I, Pohlen, M, Rangwala, N, Roseboom, IG, Rowan-Robinson, M, Portal, MS, Schulz, B, Scott, D, Seymour, N, Shupe, D, Smith, AJ, Stevens, J, Symeonidis, M, Trichas, M, Tugwell, KE, Vaccari, M, Valiante, E, Valtchanov, I, Vieira, J, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, CK & Zemcov, M 2011, 'Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses', Nature, vol. 470, no. 7335, pp. 510-512. https://doi.org/10.1038/nature09771

TY - JOUR

T1 - Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses

AU - Amblard, A.

AU - Cooray, A.

AU - Serra, P.

AU - Altieri, B.

AU - Arumugam, V.

AU - Aussel, H.

AU - Blain, A.

AU - Bock, J.

AU - Boselli, A.

AU - Buat, V.

AU - Castro-Rodriguez, N.

AU - Cava, A.

AU - Chanial, P.

AU - Chapin, E.

AU - Clements, D.

AU - Conley, A.

AU - Conversi, L.

AU - Dowell, C.D.

AU - Dwek, E.

AU - Eales, S.

AU - Elbaz, D.

AU - Farrah, D.

AU - Franceschini, A.

AU - Gear, W.K.

AU - Glenn, J.

AU - Griffin, M.

AU - Halpern, M.

AU - Hatziminaoglou, E.

AU - Ibar, E.

AU - Isaak, K.G.

AU - Ivison, R.J.

AU - Khostovan, A.A.

AU - Lagache, G.

AU - Levenson, L.

AU - Lu, N.

AU - Madden, S.

AU - Maffei, B.

AU - Mainetti, G.

AU - Marchetti, L.

AU - Marsden, G.

AU - Mitchell-Wynne, K.

AU - Nguyen, H.T.

AU - O'Halloran, B.

AU - Oliver, S.

AU - Omont, A.

AU - Page, M.J.

AU - Panuzzo, P.

AU - Papageorgiou, A.

AU - Pearson, C.P.

AU - Perez-Fournon, I.

AU - Pohlen, M.

AU - Rangwala, N.

AU - Roseboom, I.G.

AU - Rowan-Robinson, M.

AU - Portal, M.S.

AU - Schulz, B.

AU - Scott, D.

AU - Seymour, N.

AU - Shupe, D.

AU - Smith, A.J.

AU - Stevens, Jason

AU - Symeonidis, M.

AU - Trichas, M.

AU - Tugwell, K.E.

AU - Vaccari, M.

AU - Valiante, E.

AU - Valtchanov, I.

AU - Vieira, J.

AU - Vigroux, L.

AU - Wang, L.

AU - Ward, R.

AU - Wright, G.

AU - Xu, C.K.

AU - Zemcov, M.

N1 - Original article can be found at: http://www.nature.com/ Copyright Nature Publishing Group

PY - 2011

Y1 - 2011

N2 - The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).

AB - The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).

KW - Herschel-spire instrument

KW - star formation

KW - number counts

KW - Hermes

KW - redshift

KW - spitzer

KW - atlas

KW - bias

U2 - 10.1038/nature09771

DO - 10.1038/nature09771

M3 - Article

SN - 0028-0836

VL - 470

SP - 510

EP - 512

JO - Nature

JF - Nature

IS - 7335

ER -

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 x 10(11) solar masses

Abstract

Keywords

Access to Document

Fingerprint

Cite this