Cluster and field elliptical galaxies at z\textasciitilde1.3. The marginal role of the environment and the relevance of the galaxy central regions. Saracco, P., Gargiulo, A., Ciocca, F., & Marchesini, D. Astronomy & Astrophysics, 597:A122, January, 2017. arXiv: 1609.06726![Cluster and field elliptical galaxies at z\textasciitilde1.3. The marginal role of the environment and the relevance of the galaxy central regions [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We compared the properties of 56 elliptical galaxies selected from three clusters at \$1.2{\textless}z{\textless}1.4\$ with those of field galaxies in the GOODS-S (\textasciitilde30), COSMOS (\textasciitilde180) and CANDELS (\textasciitilde220) fields. We studied the relationships among effective radius, surface brightness, stellar mass, stellar mass density \${\textbackslash}Sigma_\{Re\}\$ and central mass density \${\textbackslash}Sigma_\{1kpc\}\$ within 1 kpc radius. We find that cluster ellipticals do not differ from field ellipticals: they share the same structural parameters at fixed mass and the same scaling relations. On the other hand, the population of field ellipticals at \$z{\textbackslash}sim1.3\$ shows a significant lack of massive (\$M_*{\textgreater} 2{\textbackslash}times 10{\textasciicircum}\{11\}\$ M\$_{\textbackslash}odot\$) and large (R\$_e {\textgreater} 4-5\$ kpc) ellipticals with respect to the cluster. Nonetheless, at \$M*{\textless}2{\textbackslash}times 10{\textasciicircum}\{11\}\$ M\$_{\textbackslash}odot\$, the two populations are similar. The size-mass relation of ellipticals at z\textasciitilde1.3 defines two different regimes, above and below a transition mass \$m_t{\textbackslash}sim 2-3{\textbackslash}times10{\textasciicircum}\{10\}\$ M\$_{\textbackslash}odot\$: at lower masses the relation is nearly flat (R\$_e{\textbackslash}propto M_*{\textasciicircum}\{-0.1{\textbackslash}pm 0.2\}\$), the mean radius is constant at \textasciitilde1 kpc and \${\textbackslash}Sigma_\{Re\}{\textbackslash}sim {\textbackslash}Sigma_\{1kpc\}\$ while, at larger masses, the relation is R\$_e{\textbackslash}propto M*{\textasciicircum}\{0.64{\textbackslash}pm0.09\}\$. The transition mass marks the mass at which galaxies reach the maximum \${\textbackslash}Sigma_\{Re\}\$. Also the \${\textbackslash}Sigma_\{1kpc\}\$-mass relation follows two different regimes, \${\textbackslash}Sigma_\{1kpc\}{\textbackslash}propto M*{\textasciicircum}\{0.64{\textbackslash} {\textgreater}m_t\}_\{1.07{\textbackslash} {\textless}m_t\}\$, defining a transition mass density \${\textbackslash}Sigma_\{1kpc\}{\textbackslash}sim 2-3{\textbackslash}times10{\textasciicircum}3\$ M\$_{\textbackslash}odot\$ pc\${\textasciicircum}\{-2\}\$. The mass density \${\textbackslash}Sigma_\{Re\}\$ does not correlate with mass, dense/compact galaxies can be assembled over a wide mass regime, independently of the environment. The central mass density, \${\textbackslash}Sigma_\{1kpc\}\$, besides to be correlated with the mass, is correlated to the age of the stellar population: the higher the central stellar mass density, the higher the mass, the older the age of the stellar population. [Abridged]
@article{saracco_cluster_2017,
title = {Cluster and field elliptical galaxies at z{\textasciitilde}1.3. {The} marginal role of the environment and the relevance of the galaxy central regions},
volume = {597},
issn = {0004-6361, 1432-0746},
url = {http://arxiv.org/abs/1609.06726},
doi = {10.1051/0004-6361/201628866},
abstract = {We compared the properties of 56 elliptical galaxies selected from three clusters at \$1.2{\textless}z{\textless}1.4\$ with those of field galaxies in the GOODS-S ({\textasciitilde}30), COSMOS ({\textasciitilde}180) and CANDELS ({\textasciitilde}220) fields. We studied the relationships among effective radius, surface brightness, stellar mass, stellar mass density \${\textbackslash}Sigma\_\{Re\}\$ and central mass density \${\textbackslash}Sigma\_\{1kpc\}\$ within 1 kpc radius. We find that cluster ellipticals do not differ from field ellipticals: they share the same structural parameters at fixed mass and the same scaling relations. On the other hand, the population of field ellipticals at \$z{\textbackslash}sim1.3\$ shows a significant lack of massive (\$M\_*{\textgreater} 2{\textbackslash}times 10{\textasciicircum}\{11\}\$ M\$\_{\textbackslash}odot\$) and large (R\$\_e {\textgreater} 4-5\$ kpc) ellipticals with respect to the cluster. Nonetheless, at \$M*{\textless}2{\textbackslash}times 10{\textasciicircum}\{11\}\$ M\$\_{\textbackslash}odot\$, the two populations are similar. The size-mass relation of ellipticals at z{\textasciitilde}1.3 defines two different regimes, above and below a transition mass \$m\_t{\textbackslash}sim 2-3{\textbackslash}times10{\textasciicircum}\{10\}\$ M\$\_{\textbackslash}odot\$: at lower masses the relation is nearly flat (R\$\_e{\textbackslash}propto M\_*{\textasciicircum}\{-0.1{\textbackslash}pm 0.2\}\$), the mean radius is constant at {\textasciitilde}1 kpc and \${\textbackslash}Sigma\_\{Re\}{\textbackslash}sim {\textbackslash}Sigma\_\{1kpc\}\$ while, at larger masses, the relation is R\$\_e{\textbackslash}propto M*{\textasciicircum}\{0.64{\textbackslash}pm0.09\}\$. The transition mass marks the mass at which galaxies reach the maximum \${\textbackslash}Sigma\_\{Re\}\$. Also the \${\textbackslash}Sigma\_\{1kpc\}\$-mass relation follows two different regimes, \${\textbackslash}Sigma\_\{1kpc\}{\textbackslash}propto M*{\textasciicircum}\{0.64{\textbackslash} {\textgreater}m\_t\}\_\{1.07{\textbackslash} {\textless}m\_t\}\$, defining a transition mass density \${\textbackslash}Sigma\_\{1kpc\}{\textbackslash}sim 2-3{\textbackslash}times10{\textasciicircum}3\$ M\$\_{\textbackslash}odot\$ pc\${\textasciicircum}\{-2\}\$. The mass density \${\textbackslash}Sigma\_\{Re\}\$ does not correlate with mass, dense/compact galaxies can be assembled over a wide mass regime, independently of the environment. The central mass density, \${\textbackslash}Sigma\_\{1kpc\}\$, besides to be correlated with the mass, is correlated to the age of the stellar population: the higher the central stellar mass density, the higher the mass, the older the age of the stellar population. [Abridged]},
journal = {Astronomy \& Astrophysics},
author = {Saracco, P. and Gargiulo, A. and Ciocca, F. and Marchesini, D.},
month = jan,
year = {2017},
note = {arXiv: 1609.06726},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {A122},
}
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{"_id":"2kR8N7ydWHfXM3FqE","bibbaseid":"saracco-gargiulo-ciocca-marchesini-clusterandfieldellipticalgalaxiesatztextasciitilde13themarginalroleoftheenvironmentandtherelevanceofthegalaxycentralregions-2017","author_short":["Saracco, P.","Gargiulo, A.","Ciocca, F.","Marchesini, D."],"bibdata":{"bibtype":"article","type":"article","title":"Cluster and field elliptical galaxies at z\\textasciitilde1.3. The marginal role of the environment and the relevance of the galaxy central regions","volume":"597","issn":"0004-6361, 1432-0746","url":"http://arxiv.org/abs/1609.06726","doi":"10.1051/0004-6361/201628866","abstract":"We compared the properties of 56 elliptical galaxies selected from three clusters at \\$1.2{\\textless}z{\\textless}1.4\\$ with those of field galaxies in the GOODS-S (\\textasciitilde30), COSMOS (\\textasciitilde180) and CANDELS (\\textasciitilde220) fields. We studied the relationships among effective radius, surface brightness, stellar mass, stellar mass density \\${\\textbackslash}Sigma_\\{Re\\}\\$ and central mass density \\${\\textbackslash}Sigma_\\{1kpc\\}\\$ within 1 kpc radius. We find that cluster ellipticals do not differ from field ellipticals: they share the same structural parameters at fixed mass and the same scaling relations. On the other hand, the population of field ellipticals at \\$z{\\textbackslash}sim1.3\\$ shows a significant lack of massive (\\$M_*{\\textgreater} 2{\\textbackslash}times 10{\\textasciicircum}\\{11\\}\\$ M\\$_{\\textbackslash}odot\\$) and large (R\\$_e {\\textgreater} 4-5\\$ kpc) ellipticals with respect to the cluster. Nonetheless, at \\$M*{\\textless}2{\\textbackslash}times 10{\\textasciicircum}\\{11\\}\\$ M\\$_{\\textbackslash}odot\\$, the two populations are similar. The size-mass relation of ellipticals at z\\textasciitilde1.3 defines two different regimes, above and below a transition mass \\$m_t{\\textbackslash}sim 2-3{\\textbackslash}times10{\\textasciicircum}\\{10\\}\\$ M\\$_{\\textbackslash}odot\\$: at lower masses the relation is nearly flat (R\\$_e{\\textbackslash}propto M_*{\\textasciicircum}\\{-0.1{\\textbackslash}pm 0.2\\}\\$), the mean radius is constant at \\textasciitilde1 kpc and \\${\\textbackslash}Sigma_\\{Re\\}{\\textbackslash}sim {\\textbackslash}Sigma_\\{1kpc\\}\\$ while, at larger masses, the relation is R\\$_e{\\textbackslash}propto M*{\\textasciicircum}\\{0.64{\\textbackslash}pm0.09\\}\\$. The transition mass marks the mass at which galaxies reach the maximum \\${\\textbackslash}Sigma_\\{Re\\}\\$. Also the \\${\\textbackslash}Sigma_\\{1kpc\\}\\$-mass relation follows two different regimes, \\${\\textbackslash}Sigma_\\{1kpc\\}{\\textbackslash}propto M*{\\textasciicircum}\\{0.64{\\textbackslash} {\\textgreater}m_t\\}_\\{1.07{\\textbackslash} {\\textless}m_t\\}\\$, defining a transition mass density \\${\\textbackslash}Sigma_\\{1kpc\\}{\\textbackslash}sim 2-3{\\textbackslash}times10{\\textasciicircum}3\\$ M\\$_{\\textbackslash}odot\\$ pc\\${\\textasciicircum}\\{-2\\}\\$. The mass density \\${\\textbackslash}Sigma_\\{Re\\}\\$ does not correlate with mass, dense/compact galaxies can be assembled over a wide mass regime, independently of the environment. The central mass density, \\${\\textbackslash}Sigma_\\{1kpc\\}\\$, besides to be correlated with the mass, is correlated to the age of the stellar population: the higher the central stellar mass density, the higher the mass, the older the age of the stellar population. [Abridged]","journal":"Astronomy & Astrophysics","author":[{"propositions":[],"lastnames":["Saracco"],"firstnames":["P."],"suffixes":[]},{"propositions":[],"lastnames":["Gargiulo"],"firstnames":["A."],"suffixes":[]},{"propositions":[],"lastnames":["Ciocca"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Marchesini"],"firstnames":["D."],"suffixes":[]}],"month":"January","year":"2017","note":"arXiv: 1609.06726","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"A122","bibtex":"@article{saracco_cluster_2017,\n\ttitle = {Cluster and field elliptical galaxies at z{\\textasciitilde}1.3. {The} marginal role of the environment and the relevance of the galaxy central regions},\n\tvolume = {597},\n\tissn = {0004-6361, 1432-0746},\n\turl = {http://arxiv.org/abs/1609.06726},\n\tdoi = {10.1051/0004-6361/201628866},\n\tabstract = {We compared the properties of 56 elliptical galaxies selected from three clusters at \\$1.2{\\textless}z{\\textless}1.4\\$ with those of field galaxies in the GOODS-S ({\\textasciitilde}30), COSMOS ({\\textasciitilde}180) and CANDELS ({\\textasciitilde}220) fields. We studied the relationships among effective radius, surface brightness, stellar mass, stellar mass density \\${\\textbackslash}Sigma\\_\\{Re\\}\\$ and central mass density \\${\\textbackslash}Sigma\\_\\{1kpc\\}\\$ within 1 kpc radius. We find that cluster ellipticals do not differ from field ellipticals: they share the same structural parameters at fixed mass and the same scaling relations. On the other hand, the population of field ellipticals at \\$z{\\textbackslash}sim1.3\\$ shows a significant lack of massive (\\$M\\_*{\\textgreater} 2{\\textbackslash}times 10{\\textasciicircum}\\{11\\}\\$ M\\$\\_{\\textbackslash}odot\\$) and large (R\\$\\_e {\\textgreater} 4-5\\$ kpc) ellipticals with respect to the cluster. Nonetheless, at \\$M*{\\textless}2{\\textbackslash}times 10{\\textasciicircum}\\{11\\}\\$ M\\$\\_{\\textbackslash}odot\\$, the two populations are similar. The size-mass relation of ellipticals at z{\\textasciitilde}1.3 defines two different regimes, above and below a transition mass \\$m\\_t{\\textbackslash}sim 2-3{\\textbackslash}times10{\\textasciicircum}\\{10\\}\\$ M\\$\\_{\\textbackslash}odot\\$: at lower masses the relation is nearly flat (R\\$\\_e{\\textbackslash}propto M\\_*{\\textasciicircum}\\{-0.1{\\textbackslash}pm 0.2\\}\\$), the mean radius is constant at {\\textasciitilde}1 kpc and \\${\\textbackslash}Sigma\\_\\{Re\\}{\\textbackslash}sim {\\textbackslash}Sigma\\_\\{1kpc\\}\\$ while, at larger masses, the relation is R\\$\\_e{\\textbackslash}propto M*{\\textasciicircum}\\{0.64{\\textbackslash}pm0.09\\}\\$. The transition mass marks the mass at which galaxies reach the maximum \\${\\textbackslash}Sigma\\_\\{Re\\}\\$. Also the \\${\\textbackslash}Sigma\\_\\{1kpc\\}\\$-mass relation follows two different regimes, \\${\\textbackslash}Sigma\\_\\{1kpc\\}{\\textbackslash}propto M*{\\textasciicircum}\\{0.64{\\textbackslash} {\\textgreater}m\\_t\\}\\_\\{1.07{\\textbackslash} {\\textless}m\\_t\\}\\$, defining a transition mass density \\${\\textbackslash}Sigma\\_\\{1kpc\\}{\\textbackslash}sim 2-3{\\textbackslash}times10{\\textasciicircum}3\\$ M\\$\\_{\\textbackslash}odot\\$ pc\\${\\textasciicircum}\\{-2\\}\\$. The mass density \\${\\textbackslash}Sigma\\_\\{Re\\}\\$ does not correlate with mass, dense/compact galaxies can be assembled over a wide mass regime, independently of the environment. The central mass density, \\${\\textbackslash}Sigma\\_\\{1kpc\\}\\$, besides to be correlated with the mass, is correlated to the age of the stellar population: the higher the central stellar mass density, the higher the mass, the older the age of the stellar population. [Abridged]},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Saracco, P. and Gargiulo, A. and Ciocca, F. and Marchesini, D.},\n\tmonth = jan,\n\tyear = {2017},\n\tnote = {arXiv: 1609.06726},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {A122},\n}\n\n","author_short":["Saracco, P.","Gargiulo, A.","Ciocca, F.","Marchesini, D."],"key":"saracco_cluster_2017","id":"saracco_cluster_2017","bibbaseid":"saracco-gargiulo-ciocca-marchesini-clusterandfieldellipticalgalaxiesatztextasciitilde13themarginalroleoftheenvironmentandtherelevanceofthegalaxycentralregions-2017","role":"author","urls":{"Paper":"http://arxiv.org/abs/1609.06726"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["cluster","field","elliptical","galaxies","textasciitilde1","marginal","role","environment","relevance","galaxy","central","regions","saracco","gargiulo","ciocca","marchesini"],"title":"Cluster and field elliptical galaxies at z\\textasciitilde1.3. The marginal role of the environment and the relevance of the galaxy central regions","year":2017}