THE FORMATION OF MASSIVE CLUSTER GALAXIES

Mancone, Conor L; Gonzalez, Anthony H; Brodwin, Mark; Jones, Christine; Stanford, Spencer A; Eisenhardt, Peter R. M.; Stern, Daniel

doi:10.1088/0004-637X/720/1/284

Title: THE FORMATION OF MASSIVE CLUSTER GALAXIES

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Abstract

We present composite 3.6 and 4.5 {mu}m luminosity functions (LFs) for cluster galaxies measured from the Spitzer Deep, Wide-Field Survey for 0.3 < z < 2. We compare the evolution of m* for these LFs to models for passively evolving stellar populations to constrain the primary epoch of star formation in massive cluster galaxies. At low redshifts (z {approx}< 1.3), our results agree well with models with no mass assembly and passively evolving stellar populations with a luminosity-weighted mean formation redshift z{sub f} = 2.4 assuming a Kroupa initial mass function (IMF). We conduct a thorough investigation of systematic biases that might influence our results, and estimate systematic uncertainties of {Delta}z{sub f} = {sup +0.16} {sub -0.18} (model normalization), {Delta}z{sub f} = {sup +0.40}{sub -0.05} ({alpha}), and {Delta}z{sub f} = {sup +0.30}{sub -0.45} (choice of stellar population model). For a Salpeter-type IMF, the typical formation epoch is thus strongly constrained to be z {approx} 2-3. Higher formation redshifts can only be made consistent with the data if one permits an evolving IMF that is bottom-light at high redshift, as suggested by van Dokkum. At high redshifts (z {approx}> 1.3), we also witness a statistically significant (>5{sigma}) disagreement between the measuredmore »« less

Authors:

Mancone, Conor L; Gonzalez, Anthony H ^[1]; Brodwin, Mark; Jones, Christine ^[2]; Stanford, Spencer A ^[3]; Eisenhardt, Peter R. M.; Stern, Daniel ^[4]

Department of Astronomy, University of Florida, Gainesville, FL 32611 (United States)
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
Physics Department, University of California, Davis, CA 95616 (United States)
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States)

Publication Date:: Wed Sep 01 00:00:00 EDT 2010

OSTI Identifier:: 21460141

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 720; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/720/1/284; Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; GALACTIC EVOLUTION; GALAXIES; GALAXY CLUSTERS; LUMINOSITY; MASS; RED SHIFT; STARS; EVOLUTION; OPTICAL PROPERTIES; PHYSICAL PROPERTIES

Citation Formats


                    Mancone, Conor L, Gonzalez, Anthony H, Brodwin, Mark, Jones, Christine, Stanford, Spencer A, Eisenhardt, Peter R. M., and Stern, Daniel. THE FORMATION OF MASSIVE CLUSTER GALAXIES.  United States: N. p., 2010. 
        Web.  doi:10.1088/0004-637X/720/1/284.

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                    Mancone, Conor L, Gonzalez, Anthony H, Brodwin, Mark, Jones, Christine, Stanford, Spencer A, Eisenhardt, Peter R. M., & Stern, Daniel. THE FORMATION OF MASSIVE CLUSTER GALAXIES.  United States.  https://doi.org/10.1088/0004-637X/720/1/284

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                    Mancone, Conor L, Gonzalez, Anthony H, Brodwin, Mark, Jones, Christine, Stanford, Spencer A, Eisenhardt, Peter R. M., and Stern, Daniel. 2010.  
        "THE FORMATION OF MASSIVE CLUSTER GALAXIES".  United States.  https://doi.org/10.1088/0004-637X/720/1/284.

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@article{osti_21460141,

  title        = {THE FORMATION OF MASSIVE CLUSTER GALAXIES},

  author       = {Mancone, Conor L and Gonzalez, Anthony H and Brodwin, Mark and Jones, Christine and Stanford, Spencer A and Eisenhardt, Peter R. M. and Stern, Daniel},

  abstractNote = {We present composite 3.6 and 4.5 {mu}m luminosity functions (LFs) for cluster galaxies measured from the Spitzer Deep, Wide-Field Survey for 0.3 < z < 2. We compare the evolution of m* for these LFs to models for passively evolving stellar populations to constrain the primary epoch of star formation in massive cluster galaxies. At low redshifts (z {approx}< 1.3), our results agree well with models with no mass assembly and passively evolving stellar populations with a luminosity-weighted mean formation redshift z{sub f} = 2.4 assuming a Kroupa initial mass function (IMF). We conduct a thorough investigation of systematic biases that might influence our results, and estimate systematic uncertainties of {Delta}z{sub f} = {sup +0.16} {sub -0.18} (model normalization), {Delta}z{sub f} = {sup +0.40}{sub -0.05} ({alpha}), and {Delta}z{sub f} = {sup +0.30}{sub -0.45} (choice of stellar population model). For a Salpeter-type IMF, the typical formation epoch is thus strongly constrained to be z {approx} 2-3. Higher formation redshifts can only be made consistent with the data if one permits an evolving IMF that is bottom-light at high redshift, as suggested by van Dokkum. At high redshifts (z {approx}> 1.3), we also witness a statistically significant (>5{sigma}) disagreement between the measured LF and the continuation of the passive evolution model from lower redshifts. After considering potential systematic biases that might influence our highest redshift data points, we interpret the observed deviation as potential evidence for ongoing mass assembly at this epoch.},

  doi          = {10.1088/0004-637X/720/1/284},

  url          = {https://www.osti.gov/biblio/21460141},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 1,

  volume       = 720,

  place        = {United States},

  year         = {Wed Sep 01 00:00:00 EDT 2010},

  month        = {Wed Sep 01 00:00:00 EDT 2010}

}

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