Abstract
We probe star formation in the environments of massive (∼1013 M☉) dark matter haloes at redshifts of z ∼ 1. This star formation is linked to a submillimetre clustering signal which we detect in maps of the Planck High Frequency Instrument that are stacked at the positions of a sample of high redshift (z > 2) strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope (SPT) 2500 deg2 survey. The clustering signal has submillimetre colours which are consistent with the mean redshift of the foreground lensing haloes (z ∼ 1). We report a mean excess of star formation rate (SFR) compared to the field, of (2700 ± 700) M☉ yr−1 from all galaxies contributing to this clustering signal within a radius of 3.5 arcmin from the SPT DSFGs. The magnitude of the Planck excess is in broad agreement with predictions of a current model of the cosmic infrared background. The model predicts that 80 per cent of the excess emission measured by Planck originates from galaxies lying in the neighbouring haloes of the lensing halo. Using Herschel maps of the same fields, we find a clear excess, relative to the field, of individual sources which contribute to the Planck excess. The mean excess SFR compared to the field is measured to be (370 ± 40) M☉ yr−1 per resolved, clustered source. Our findings suggest that the environments around these massive z ∼ 1 lensing haloes host intense star formation out to about 2 Mpc. The flux enhancement due to clustering should also be considered when measuring flux densities of galaxies in Planck data.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 1629-1646 |
| Number of pages | 18 |
| Journal | Monthly Notices of the Royal Astronomical Society: Letters |
| Volume | 455 |
| Issue number | 2 |
| DOIs | |
| State | Published - Jan 1 2020 |
Keywords
- Diffuse radiation
- Galaxies: formation
- Galaxies: statistics
- Submillimetre: galaxies
- Surveys
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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Probing star formation in the dense environments of z ∼ 1 lensing haloes aligned with dusty star-forming galaxies detected with the South Pole telescope. / Welikala, N.; Béthermin, M.; Guery, D.; Strandet, M.; Aird, K. A.; Aravena, M.; Ashby, M. L.N.; Bothwell, M.; Beelen, A.; Bleem, L. E.; de Breuck, C.; Brodwin, M.; Carlstrom, J. E.; Chapman, S. C.; Crawford, T. M.; Dole, H.; Doré, O.; Everett, W.; Flores-Cacho, I.; Gonzalez, A. H.; González-Nuevo, J.; Greve, T. R.; Gullberg, B.; Hezaveh, Y. D.; Holder, G. P.; Holzapfel, W. L.; Keisler, R.; Lagache, G.; Ma, J.; Malkan, M.; Marrone, D. P.; Mocanu, L. M.; Montier, L.; Murphy, E. J.; Nesvadba, N. P.H.; Omont, A.; Pointecouteau, E.; Puget, J. L.; Reichardt, C. L.; Rotermund, K. M.; Scott, D.; Serra, P.; Spilker, J. S.; Stalder, B.; Stark, A. A.; Story, K.; Vanderlinde, K.; Vieira, J. D.; Weiß, A.
In: Monthly Notices of the Royal Astronomical Society: Letters, Vol. 455, No. 2, 01.01.2020, p. 1629-1646.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Probing star formation in the dense environments of z ∼ 1 lensing haloes aligned with dusty star-forming galaxies detected with the South Pole telescope
AU - Welikala, N.
AU - Béthermin, M.
AU - Guery, D.
AU - Strandet, M.
AU - Aird, K. A.
AU - Aravena, M.
AU - Ashby, M. L.N.
AU - Bothwell, M.
AU - Beelen, A.
AU - Bleem, L. E.
AU - de Breuck, C.
AU - Brodwin, M.
AU - Carlstrom, J. E.
AU - Chapman, S. C.
AU - Crawford, T. M.
AU - Dole, H.
AU - Doré, O.
AU - Everett, W.
AU - Flores-Cacho, I.
AU - Gonzalez, A. H.
AU - González-Nuevo, J.
AU - Greve, T. R.
AU - Gullberg, B.
AU - Hezaveh, Y. D.
AU - Holder, G. P.
AU - Holzapfel, W. L.
AU - Keisler, R.
AU - Lagache, G.
AU - Ma, J.
AU - Malkan, M.
AU - Marrone, D. P.
AU - Mocanu, L. M.
AU - Montier, L.
AU - Murphy, E. J.
AU - Nesvadba, N. P.H.
AU - Omont, A.
AU - Pointecouteau, E.
AU - Puget, J. L.
AU - Reichardt, C. L.
AU - Rotermund, K. M.
AU - Scott, D.
AU - Serra, P.
AU - Spilker, J. S.
AU - Stalder, B.
AU - Stark, A. A.
AU - Story, K.
AU - Vanderlinde, K.
AU - Vieira, J. D.
AU - Weiß, A.
N1 - Funding Information: We thank the anonymous referee for valuable comments. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. This paper is based on work supported by the US National Science Foundation under grant no. AST-1312950. Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page= PlanckCollaboration. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00957.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. APEX is a collaboration between the Max-Planck-Institut f?r Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA, and supported through an award issued by JPL/Caltech for OT2_jvieira_5. NW acknowledges support from the Beecroft Institute for Particle Astrophysics and Cosmology and previous support from the Centre National d'?tudes Spatiales (CNES). Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. MS was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. IF-C acknowledges the support of grant ANR-11-BS56-015. JG-N acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, cofunded by the European Social Fund, by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects. NW thanks B. Partridge, J. Delabrouille, D. Harrison, and P. Vielva for useful comments. Funding Information: We thank the anonymous referee for valuable comments. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. This paper is based on work supported by the US National Science Foundation under grant no. AST-1312950. Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page= PlanckCollaboration. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00957.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. APEX is a collaboration between the Max-Planck-Institut für Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA, and supported through an award issued by JPL/Caltech for OT2_jvieira_5. NW acknowledges support from the Beecroft Institute for Particle Astrophysics and Cosmology and previous support from the Centre National d’Études Spatiales (CNES). Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. MS was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. IF-C acknowledges the support of grant ANR-11-BS56-015. JG-N acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, cofunded by the European Social Fund, by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects. NW thanks B. Partridge, J. Delabrouille, D. Harrison, and P. Vielva for useful comments. Publisher Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
PY - 2020/1/1
Y1 - 2020/1/1
N2 - We probe star formation in the environments of massive (∼1013 M☉) dark matter haloes at redshifts of z ∼ 1. This star formation is linked to a submillimetre clustering signal which we detect in maps of the Planck High Frequency Instrument that are stacked at the positions of a sample of high redshift (z > 2) strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope (SPT) 2500 deg2 survey. The clustering signal has submillimetre colours which are consistent with the mean redshift of the foreground lensing haloes (z ∼ 1). We report a mean excess of star formation rate (SFR) compared to the field, of (2700 ± 700) M☉ yr−1 from all galaxies contributing to this clustering signal within a radius of 3.5 arcmin from the SPT DSFGs. The magnitude of the Planck excess is in broad agreement with predictions of a current model of the cosmic infrared background. The model predicts that 80 per cent of the excess emission measured by Planck originates from galaxies lying in the neighbouring haloes of the lensing halo. Using Herschel maps of the same fields, we find a clear excess, relative to the field, of individual sources which contribute to the Planck excess. The mean excess SFR compared to the field is measured to be (370 ± 40) M☉ yr−1 per resolved, clustered source. Our findings suggest that the environments around these massive z ∼ 1 lensing haloes host intense star formation out to about 2 Mpc. The flux enhancement due to clustering should also be considered when measuring flux densities of galaxies in Planck data.
AB - We probe star formation in the environments of massive (∼1013 M☉) dark matter haloes at redshifts of z ∼ 1. This star formation is linked to a submillimetre clustering signal which we detect in maps of the Planck High Frequency Instrument that are stacked at the positions of a sample of high redshift (z > 2) strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope (SPT) 2500 deg2 survey. The clustering signal has submillimetre colours which are consistent with the mean redshift of the foreground lensing haloes (z ∼ 1). We report a mean excess of star formation rate (SFR) compared to the field, of (2700 ± 700) M☉ yr−1 from all galaxies contributing to this clustering signal within a radius of 3.5 arcmin from the SPT DSFGs. The magnitude of the Planck excess is in broad agreement with predictions of a current model of the cosmic infrared background. The model predicts that 80 per cent of the excess emission measured by Planck originates from galaxies lying in the neighbouring haloes of the lensing halo. Using Herschel maps of the same fields, we find a clear excess, relative to the field, of individual sources which contribute to the Planck excess. The mean excess SFR compared to the field is measured to be (370 ± 40) M☉ yr−1 per resolved, clustered source. Our findings suggest that the environments around these massive z ∼ 1 lensing haloes host intense star formation out to about 2 Mpc. The flux enhancement due to clustering should also be considered when measuring flux densities of galaxies in Planck data.
KW - Diffuse radiation
KW - Galaxies: formation
KW - Galaxies: statistics
KW - Submillimetre: galaxies
KW - Surveys
UR - http://www.scopus.com/inward/record.url?scp=85088498256&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85088498256&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv2302
DO - 10.1093/mnras/stv2302
M3 - Article
AN - SCOPUS:85088498256
VL - 455
SP - 1629
EP - 1646
JO - Monthly Notices of the Royal Astronomical Society: Letters
JF - Monthly Notices of the Royal Astronomical Society: Letters
SN - 1745-3933
IS - 2
ER -