Matches in SemOpenAlex for { <https://semopenalex.org/work/W2015353002> ?p ?o ?g. }
- W2015353002 endingPage "1182" @default.
- W2015353002 startingPage "1163" @default.
- W2015353002 abstract "We report on the X-ray evolution over the last ≈9 Gyr of cosmic history (i.e., since z = 1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ≈5-10) in the X-ray-to-optical mean luminosity ratio (LX/LB) and the X-ray-to-stellar mass mean ratio (LX/M⋆) for galaxy populations selected by LB and M⋆, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (LX/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR = 1-100 M☉ yr−1, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z ≈ 1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z = 0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z ∼ 3 and estimate that LX/LB at z ∼ 3 is similar to its value at z = 1.4." @default.
- W2015353002 created "2016-06-24" @default.
- W2015353002 creator A5003374647 @default.
- W2015353002 creator A5008915976 @default.
- W2015353002 creator A5012352257 @default.
- W2015353002 creator A5015491870 @default.
- W2015353002 creator A5015837326 @default.
- W2015353002 creator A5024335460 @default.
- W2015353002 creator A5025718836 @default.
- W2015353002 creator A5035495817 @default.
- W2015353002 creator A5047186596 @default.
- W2015353002 creator A5066116709 @default.
- W2015353002 creator A5073154205 @default.
- W2015353002 creator A5076386690 @default.
- W2015353002 creator A5079781692 @default.
- W2015353002 creator A5082749953 @default.
- W2015353002 date "2008-07-10" @default.
- W2015353002 modified "2023-10-03" @default.
- W2015353002 title "Tracing the Mass‐Dependent Star Formation History of Late‐Type Galaxies Using X‐Ray Emission: Results from the Chandra Deep Fields" @default.
- W2015353002 cites W1497175568 @default.
- W2015353002 cites W1607434071 @default.
- W2015353002 cites W1614298107 @default.
- W2015353002 cites W1651990138 @default.
- W2015353002 cites W1787231361 @default.
- W2015353002 cites W1963787353 @default.
- W2015353002 cites W1965539998 @default.
- W2015353002 cites W1966609605 @default.
- W2015353002 cites W1970440163 @default.
- W2015353002 cites W1972005805 @default.
- W2015353002 cites W1972308849 @default.
- W2015353002 cites W1973085296 @default.
- W2015353002 cites W1976615408 @default.
- W2015353002 cites W1977088063 @default.
- W2015353002 cites W1977376891 @default.
- W2015353002 cites W1980904486 @default.
- W2015353002 cites W1982563147 @default.
- W2015353002 cites W1989738078 @default.
- W2015353002 cites W1990060263 @default.
- W2015353002 cites W1996755716 @default.
- W2015353002 cites W1997313837 @default.
- W2015353002 cites W1998981512 @default.
- W2015353002 cites W2002015260 @default.
- W2015353002 cites W2007649291 @default.
- W2015353002 cites W2008040156 @default.
- W2015353002 cites W2009489905 @default.
- W2015353002 cites W2014203224 @default.
- W2015353002 cites W2015269788 @default.
- W2015353002 cites W2017450908 @default.
- W2015353002 cites W2018388366 @default.
- W2015353002 cites W2025155866 @default.
- W2015353002 cites W2025183738 @default.
- W2015353002 cites W2026413257 @default.
- W2015353002 cites W2027258334 @default.
- W2015353002 cites W2027744705 @default.
- W2015353002 cites W2028093813 @default.
- W2015353002 cites W2029965202 @default.
- W2015353002 cites W2031670668 @default.
- W2015353002 cites W2033731878 @default.
- W2015353002 cites W2035304216 @default.
- W2015353002 cites W2036067268 @default.
- W2015353002 cites W2038434077 @default.
- W2015353002 cites W2044572891 @default.
- W2015353002 cites W2044669640 @default.
- W2015353002 cites W2046303393 @default.
- W2015353002 cites W2048186190 @default.
- W2015353002 cites W2061651748 @default.
- W2015353002 cites W2062564904 @default.
- W2015353002 cites W2063882278 @default.
- W2015353002 cites W2064179345 @default.
- W2015353002 cites W2066202006 @default.
- W2015353002 cites W2066773429 @default.
- W2015353002 cites W2069364391 @default.
- W2015353002 cites W2069896074 @default.
- W2015353002 cites W2071203866 @default.
- W2015353002 cites W2074320758 @default.
- W2015353002 cites W2079227246 @default.
- W2015353002 cites W2082129016 @default.
- W2015353002 cites W2082266584 @default.
- W2015353002 cites W2083928278 @default.
- W2015353002 cites W2084703198 @default.
- W2015353002 cites W2086879135 @default.
- W2015353002 cites W2089107762 @default.
- W2015353002 cites W2095377326 @default.
- W2015353002 cites W2095917766 @default.
- W2015353002 cites W2096290973 @default.
- W2015353002 cites W2098317144 @default.
- W2015353002 cites W2099093893 @default.
- W2015353002 cites W2102519805 @default.
- W2015353002 cites W2103263072 @default.
- W2015353002 cites W2103924419 @default.
- W2015353002 cites W2104403548 @default.
- W2015353002 cites W2104441523 @default.
- W2015353002 cites W2107337450 @default.
- W2015353002 cites W2108179281 @default.
- W2015353002 cites W2110974947 @default.
- W2015353002 cites W2111186263 @default.
- W2015353002 cites W2113504296 @default.
- W2015353002 cites W2116996962 @default.