The stellar mass function and star formation rate–stellar mass relation of galaxies at z ∼ 4–7
We investigate the evolution of the star formation rate–stellar mass relation (SFR–M ⋆) and galaxy stellar mass function (GSMF) of z ∼ 4–7 galaxies, using cosmological simulations run with the smoothed particle hydrodynamics code P-GADGET3(XXL). We explore the effects of different feedback prescript...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2015-04, Vol.448 (4), p.3001-3021 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Katsianis, A. Tescari, E. Wyithe, J. S. B. |
| description | We investigate the evolution of the star formation rate–stellar mass relation (SFR–M
⋆) and galaxy stellar mass function (GSMF) of z ∼ 4–7 galaxies, using cosmological simulations run with the smoothed particle hydrodynamics code P-GADGET3(XXL). We explore the effects of different feedback prescriptions (supernova-driven galactic winds and AGN feedback), initial stellar mass functions and metal cooling. We show that our fiducial model, with strong energy-driven winds and early active galactic nuclei (AGN) feedback, is able to reproduce the observed stellar mass function obtained from Lyman-break selected samples of star-forming galaxies at redshift 6 ≤ z ≤ 7. At z ∼ 4, observed estimates of the GSMF vary according to how the sample was selected. Our simulations are more consistent with recent results from K-selected samples, which provide a better proxy of stellar masses and are more complete at the high-mass end of the distribution. We find that in some cases simulated and observed SFR–M
⋆ relations are in tension, and this can lead to numerical predictions for the GSMF in excess of the GSMF observed. By combining the simulated SFR(M
⋆) relationship with the observed star formation rate function at a given redshift, we argue that this disagreement may be the result of the uncertainty in the SFR–M
⋆ (L
UV–M
⋆) conversion. Our simulations predict a population of faint galaxies not seen by current observations. |
| doi_str_mv | 10.1093/mnras/stv160 |
| format | Article |
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⋆ relations are in tension, and this can lead to numerical predictions for the GSMF in excess of the GSMF observed. By combining the simulated SFR(M
⋆) relationship with the observed star formation rate function at a given redshift, we argue that this disagreement may be the result of the uncertainty in the SFR–M
⋆ (L
UV–M
⋆) conversion. Our simulations predict a population of faint galaxies not seen by current observations.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stv160</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Active galactic nuclei ; Astronomy ; Computer simulation ; Cooling ; Feedback ; Galaxies ; Mathematical analysis ; Mathematical models ; Red shift ; Simulation ; Star & galaxy formation ; Star formation ; Stars & galaxies ; Stellar mass</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2015-04, Vol.448 (4), p.3001-3021</ispartof><rights>2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015</rights><rights>Copyright Oxford University Press, UK Apr 21, 2015</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c3800-1276c2b3dd4e7a94b61d85446cb823f677f496587610b81684dbee376277c7943</citedby><cites>FETCH-LOGICAL-c3800-1276c2b3dd4e7a94b61d85446cb823f677f496587610b81684dbee376277c7943</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stv160$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Katsianis, A.</creatorcontrib><creatorcontrib>Tescari, E.</creatorcontrib><creatorcontrib>Wyithe, J. S. B.</creatorcontrib><title>The stellar mass function and star formation rate–stellar mass relation of galaxies at z ∼ 4–7</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>We investigate the evolution of the star formation rate–stellar mass relation (SFR–M
⋆) and galaxy stellar mass function (GSMF) of z ∼ 4–7 galaxies, using cosmological simulations run with the smoothed particle hydrodynamics code P-GADGET3(XXL). We explore the effects of different feedback prescriptions (supernova-driven galactic winds and AGN feedback), initial stellar mass functions and metal cooling. We show that our fiducial model, with strong energy-driven winds and early active galactic nuclei (AGN) feedback, is able to reproduce the observed stellar mass function obtained from Lyman-break selected samples of star-forming galaxies at redshift 6 ≤ z ≤ 7. At z ∼ 4, observed estimates of the GSMF vary according to how the sample was selected. Our simulations are more consistent with recent results from K-selected samples, which provide a better proxy of stellar masses and are more complete at the high-mass end of the distribution. We find that in some cases simulated and observed SFR–M
⋆ relations are in tension, and this can lead to numerical predictions for the GSMF in excess of the GSMF observed. By combining the simulated SFR(M
⋆) relationship with the observed star formation rate function at a given redshift, we argue that this disagreement may be the result of the uncertainty in the SFR–M
⋆ (L
UV–M
⋆) conversion. Our simulations predict a population of faint galaxies not seen by current observations.</description><subject>Active galactic nuclei</subject><subject>Astronomy</subject><subject>Computer simulation</subject><subject>Cooling</subject><subject>Feedback</subject><subject>Galaxies</subject><subject>Mathematical analysis</subject><subject>Mathematical models</subject><subject>Red shift</subject><subject>Simulation</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars & galaxies</subject><subject>Stellar mass</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqN0b1OwzAQB3ALgUQpbDxAJAYYCLXj7xFVfEmVWMocOYkNqZK42AkCJkZ2XqAPwtRH6ZPgNiwwIKaT7n4-nfUH4BDBMwQlHtWNU37k2yfE4BYYIMxonEjGtsEAQkxjwRHaBXvezyCEBCdsAMz0QUe-1VWlXFQr7yPTNXlb2iZSTREmoW2sq9Wm5VSrV28fP7zTVT-0JrpXlXoutY9UG70uF6v3z-WChAd8H-wYVXl98F2H4O7yYjq-jie3Vzfj80mcYwFhjBLO8iTDRUE0V5JkDBWCEsLyTCTYMM4NkYwKzhDMBGKCFJnWmLOE85xLgofgpN87d_ax075N69Ln62sbbTuforBCEsax-A_FWCZSrunRLzqznWvCR4JilHJMCA3qtFe5s947bdK5K2vlXlIE03U-6SaftM8n8OOe227-t_wCVMuVcw</recordid><startdate>20150421</startdate><enddate>20150421</enddate><creator>Katsianis, A.</creator><creator>Tescari, E.</creator><creator>Wyithe, J. S. B.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20150421</creationdate><title>The stellar mass function and star formation rate–stellar mass relation of galaxies at z ∼ 4–7</title><author>Katsianis, A. ; Tescari, E. ; Wyithe, J. S. B.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c3800-1276c2b3dd4e7a94b61d85446cb823f677f496587610b81684dbee376277c7943</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Active galactic nuclei</topic><topic>Astronomy</topic><topic>Computer simulation</topic><topic>Cooling</topic><topic>Feedback</topic><topic>Galaxies</topic><topic>Mathematical analysis</topic><topic>Mathematical models</topic><topic>Red shift</topic><topic>Simulation</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars & galaxies</topic><topic>Stellar mass</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Katsianis, A.</creatorcontrib><creatorcontrib>Tescari, E.</creatorcontrib><creatorcontrib>Wyithe, J. S. B.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Katsianis, A.</au><au>Tescari, E.</au><au>Wyithe, J. S. B.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The stellar mass function and star formation rate–stellar mass relation of galaxies at z ∼ 4–7</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2015-04-21</date><risdate>2015</risdate><volume>448</volume><issue>4</issue><spage>3001</spage><epage>3021</epage><pages>3001-3021</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We investigate the evolution of the star formation rate–stellar mass relation (SFR–M
⋆) and galaxy stellar mass function (GSMF) of z ∼ 4–7 galaxies, using cosmological simulations run with the smoothed particle hydrodynamics code P-GADGET3(XXL). We explore the effects of different feedback prescriptions (supernova-driven galactic winds and AGN feedback), initial stellar mass functions and metal cooling. We show that our fiducial model, with strong energy-driven winds and early active galactic nuclei (AGN) feedback, is able to reproduce the observed stellar mass function obtained from Lyman-break selected samples of star-forming galaxies at redshift 6 ≤ z ≤ 7. At z ∼ 4, observed estimates of the GSMF vary according to how the sample was selected. Our simulations are more consistent with recent results from K-selected samples, which provide a better proxy of stellar masses and are more complete at the high-mass end of the distribution. We find that in some cases simulated and observed SFR–M
⋆ relations are in tension, and this can lead to numerical predictions for the GSMF in excess of the GSMF observed. By combining the simulated SFR(M
⋆) relationship with the observed star formation rate function at a given redshift, we argue that this disagreement may be the result of the uncertainty in the SFR–M
⋆ (L
UV–M
⋆) conversion. Our simulations predict a population of faint galaxies not seen by current observations.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stv160</doi><tpages>21</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Active galactic nuclei Astronomy Computer simulation Cooling Feedback Galaxies Mathematical analysis Mathematical models Red shift Simulation Star & galaxy formation Star formation Stars & galaxies Stellar mass |
| title | The stellar mass function and star formation rate–stellar mass relation of galaxies at z ∼ 4–7 |
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