Efficient satellite quenching at z~1 from the GEEC2 spectroscopic survey of galaxy groups
We present deep GMOS-S spectroscopy for 11 galaxy groups at 0.8
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| creator | Mok, Angus Balogh, Michael L McGee, Sean L Wilman, David J Finoguenov, Alexis Tanaka, Masayuki Giodini, Stefania Bower, Richard G Connelly, Jennifer L Hou, Annie Mulchaey, John S Parker, Laura C |
| description | We present deep GMOS-S spectroscopy for 11 galaxy groups at 0.8 |
| doi_str_mv | 10.48550/arxiv.1302.2562 |
| format | Article |
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Our sample is highly complete (>66%) for eight of the eleven groups. Using an optical-NIR colour-colour diagram, the galaxies in the sample were separated with a dust insensitive method into three categories: passive (red), star-forming (blue), and intermediate (green). The strongest environmental dependence is observed in the fraction of passive galaxies, which make up only ~20 per cent of the field in the mass range 10^{10.3}<M_{star}/M_\odot<10^{11.0} but are the dominant component of groups. If we assume that the properties of the field are similar to those of the `pre-accreted' population, the environment quenching efficiency (\epsilon_\rho) is defined as the fraction of field galaxies required to be quenched in order to match the observed red fraction inside groups. The efficiency obtained is ~0.4, similar to its value in intermediate-density environments locally. While green (intermediate) galaxies represent ~20 per cent of the star-forming population in both the group and field, at all stellar masses, the average sSFR of the group population is lower by a factor of ~3. The green population does not show strong H-delta absorption that is characteristic of starburst galaxies. Finally, the high fraction of passive galaxies in groups, when combined with satellite accretion models, require that most accreted galaxies have been affected by their environment. Thus, any delay between accretion and the onset of truncation of star formation (\tau) must be <2 Gyr, shorter than the 3-7 Gyr required to fit data at z=0. The relatively small fraction of intermediate galaxies requires that the actual quenching process occurs quickly, with an exponential decay timescale of \tau_q<1 Gyr.]]></description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1302.2562</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Astronomical models ; Color ; Cosmic dust ; Dependence ; Deposition ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Population ; Quenching ; Star & galaxy formation ; Star formation ; Starburst galaxies ; Stars & galaxies</subject><ispartof>arXiv.org, 2013-02</ispartof><rights>2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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Our sample is highly complete (>66%) for eight of the eleven groups. Using an optical-NIR colour-colour diagram, the galaxies in the sample were separated with a dust insensitive method into three categories: passive (red), star-forming (blue), and intermediate (green). The strongest environmental dependence is observed in the fraction of passive galaxies, which make up only ~20 per cent of the field in the mass range 10^{10.3}<M_{star}/M_\odot<10^{11.0} but are the dominant component of groups. If we assume that the properties of the field are similar to those of the `pre-accreted' population, the environment quenching efficiency (\epsilon_\rho) is defined as the fraction of field galaxies required to be quenched in order to match the observed red fraction inside groups. The efficiency obtained is ~0.4, similar to its value in intermediate-density environments locally. While green (intermediate) galaxies represent ~20 per cent of the star-forming population in both the group and field, at all stellar masses, the average sSFR of the group population is lower by a factor of ~3. The green population does not show strong H-delta absorption that is characteristic of starburst galaxies. Finally, the high fraction of passive galaxies in groups, when combined with satellite accretion models, require that most accreted galaxies have been affected by their environment. Thus, any delay between accretion and the onset of truncation of star formation (\tau) must be <2 Gyr, shorter than the 3-7 Gyr required to fit data at z=0. The relatively small fraction of intermediate galaxies requires that the actual quenching process occurs quickly, with an exponential decay timescale of \tau_q<1 Gyr.]]></description><subject>Astronomical models</subject><subject>Color</subject><subject>Cosmic dust</subject><subject>Dependence</subject><subject>Deposition</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Population</subject><subject>Quenching</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Starburst galaxies</subject><subject>Stars & galaxies</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotz71LAzEABfAgCJba3UkCzlfznXSUclah4NLF6Ujz0aZcL2eSK62Df7utdXrL4_F-ADxgNGWKc_Ss0zEcppgiMiVckBswIpTiSjFC7sAk5x1CiAhJOKcj8Fl7H0xwXYFZF9e2oTj4NbjObEO3gbrA7x8MfYp7WLYOLup6TmDunSkpZhP7YGAe0sGdYPRwo1t9PMFNikOf78Gt1212k_8cg9VrvZq_VcuPxfv8ZVlpjnFFkMZipriyam2R5JRpxwUWxgqMGDOeS0WdFcRaKpmS3Bg7c1LL9VrNhMd0DB6vs3_spk9hr9OpufCbC_9ceLoW-hTPsFyaXRxSd77UEKQoEkwRTH8BLZxc8Q</recordid><startdate>20130211</startdate><enddate>20130211</enddate><creator>Mok, Angus</creator><creator>Balogh, Michael L</creator><creator>McGee, Sean L</creator><creator>Wilman, David J</creator><creator>Finoguenov, Alexis</creator><creator>Tanaka, Masayuki</creator><creator>Giodini, Stefania</creator><creator>Bower, Richard G</creator><creator>Connelly, Jennifer L</creator><creator>Hou, Annie</creator><creator>Mulchaey, John S</creator><creator>Parker, Laura C</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20130211</creationdate><title>Efficient satellite quenching at z~1 from the GEEC2 spectroscopic survey of galaxy groups</title><author>Mok, Angus ; Balogh, Michael L ; McGee, Sean L ; Wilman, David J ; Finoguenov, Alexis ; Tanaka, Masayuki ; Giodini, Stefania ; Bower, Richard G ; Connelly, Jennifer L ; Hou, Annie ; Mulchaey, John S ; Parker, Laura C</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a511-20a169858d8bd07534ae5616cd61044cf5783ed62dd374875ccd9e7a7bb896f13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Astronomical models</topic><topic>Color</topic><topic>Cosmic dust</topic><topic>Dependence</topic><topic>Deposition</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Population</topic><topic>Quenching</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Starburst galaxies</topic><topic>Stars & galaxies</topic><toplevel>online_resources</toplevel><creatorcontrib>Mok, Angus</creatorcontrib><creatorcontrib>Balogh, Michael L</creatorcontrib><creatorcontrib>McGee, Sean L</creatorcontrib><creatorcontrib>Wilman, David J</creatorcontrib><creatorcontrib>Finoguenov, Alexis</creatorcontrib><creatorcontrib>Tanaka, Masayuki</creatorcontrib><creatorcontrib>Giodini, Stefania</creatorcontrib><creatorcontrib>Bower, Richard G</creatorcontrib><creatorcontrib>Connelly, Jennifer L</creatorcontrib><creatorcontrib>Hou, Annie</creatorcontrib><creatorcontrib>Mulchaey, John S</creatorcontrib><creatorcontrib>Parker, Laura C</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection (ProQuest)</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mok, Angus</au><au>Balogh, Michael L</au><au>McGee, Sean L</au><au>Wilman, David J</au><au>Finoguenov, Alexis</au><au>Tanaka, Masayuki</au><au>Giodini, Stefania</au><au>Bower, Richard G</au><au>Connelly, Jennifer L</au><au>Hou, Annie</au><au>Mulchaey, John S</au><au>Parker, Laura C</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Efficient satellite quenching at z~1 from the GEEC2 spectroscopic survey of galaxy groups</atitle><jtitle>arXiv.org</jtitle><date>2013-02-11</date><risdate>2013</risdate><eissn>2331-8422</eissn><abstract><![CDATA[We present deep GMOS-S spectroscopy for 11 galaxy groups at 0.8<z<1.0, for galaxies with r_{AB}<24.75. Our sample is highly complete (>66%) for eight of the eleven groups. Using an optical-NIR colour-colour diagram, the galaxies in the sample were separated with a dust insensitive method into three categories: passive (red), star-forming (blue), and intermediate (green). The strongest environmental dependence is observed in the fraction of passive galaxies, which make up only ~20 per cent of the field in the mass range 10^{10.3}<M_{star}/M_\odot<10^{11.0} but are the dominant component of groups. If we assume that the properties of the field are similar to those of the `pre-accreted' population, the environment quenching efficiency (\epsilon_\rho) is defined as the fraction of field galaxies required to be quenched in order to match the observed red fraction inside groups. The efficiency obtained is ~0.4, similar to its value in intermediate-density environments locally. While green (intermediate) galaxies represent ~20 per cent of the star-forming population in both the group and field, at all stellar masses, the average sSFR of the group population is lower by a factor of ~3. The green population does not show strong H-delta absorption that is characteristic of starburst galaxies. Finally, the high fraction of passive galaxies in groups, when combined with satellite accretion models, require that most accreted galaxies have been affected by their environment. Thus, any delay between accretion and the onset of truncation of star formation (\tau) must be <2 Gyr, shorter than the 3-7 Gyr required to fit data at z=0. The relatively small fraction of intermediate galaxies requires that the actual quenching process occurs quickly, with an exponential decay timescale of \tau_q<1 Gyr.]]></abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1302.2562</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Astronomical models Color Cosmic dust Dependence Deposition Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Population Quenching Star & galaxy formation Star formation Starburst galaxies Stars & galaxies |
| title | Efficient satellite quenching at z~1 from the GEEC2 spectroscopic survey of galaxy groups |
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