Matches in SemOpenAlex for { <https://semopenalex.org/work/W2034662724> ?p ?o ?g. }
- W2034662724 endingPage "53" @default.
- W2034662724 startingPage "53" @default.
- W2034662724 abstract "We study the star formation rates (SFRs) of galaxies as a function of local galaxy density at 0.6 < z < 0.9. We used a low-dispersion prism in IMACS on the 6.5 m Baade (Magellan I) telescope to obtain spectra and measured redshifts to a precision of σz/(1 + z) ∼ 1% for galaxies with zAB < 23.3 mag. We utilized a stellar mass-limited sample of 977 galaxies above M > 1.8 × 1010 M☉ (log M/M☉ >10.25) to conduct our main analysis. With three different SFR indicators, (1) Spitzer MIPS 24 μm imaging, (2) spectral energy distribution (SED) fitting, and (3) [O ii]λ3727 emission, we find the median specific SFR (SSFR) and SFR to decline from the low-density field to the cores of groups and a rich cluster. For the SED- and [O ii]-based SFRs, the decline in SSFR is roughly an order of magnitude while for the MIPS-based SFRs, the decline is a factor of ∼4. We find approximately the same magnitude of decline in SSFR even after removing the sample of galaxies near the cluster. Galaxies in groups and a cluster at these redshifts therefore have lower star formation (SF) activity than galaxies in the field, as is the case at z ∼ 0. We investigated whether the decline in SFR with increasing density is caused by a change in the proportion of quiescent and star-forming galaxies (SFGs) or by a decline in the SFRs of SFGs. Using the rest-frame U − V and V − J colors to distinguish quiescent galaxies from SFGs (including both unattenuated blue galaxies and reddened ones), we find that the fraction of quiescent galaxies increases from ∼32% to 79% from low to high density. In addition, we find the SSFRs of SFGs, selected based on U − V and V − J colors, to decline with increasing density by factors of ∼5–6 for the SED- and [O ii]-based SFRs. The MIPS-based SSFRs for SFGs decline with a shallower slope. The declining SFRs of SFGs with density are paralleled by a decline in the median AV, providing indirect evidence that the cold gas content that fuels future SF is diminished in higher density environments. The order of magnitude decline in the SSFR–density relation at 0.6 < z < 0.9 is therefore driven by both a combination of declining SFRs of SFGs as well as a changing mix of SFGs and quiescent galaxies." @default.
- W2034662724 created "2016-06-24" @default.
- W2034662724 creator A5013271839 @default.
- W2034662724 creator A5015193232 @default.
- W2034662724 creator A5038271103 @default.
- W2034662724 creator A5043074702 @default.
- W2034662724 creator A5084948126 @default.
- W2034662724 date "2011-06-16" @default.
- W2034662724 modified "2023-10-16" @default.
- W2034662724 title "THE STAR-FORMATION-RATE-DENSITY RELATION AT 0.6 <<i>z</i>< 0.9 AND THE ROLE OF STAR-FORMING GALAXIES $^,$ $^,$ $^,$ $^,$" @default.
- W2034662724 cites W1607434071 @default.
- W2034662724 cites W1815960455 @default.
- W2034662724 cites W1825093183 @default.
- W2034662724 cites W1826794997 @default.
- W2034662724 cites W1862435286 @default.
- W2034662724 cites W1916061238 @default.
- W2034662724 cites W1963501671 @default.
- W2034662724 cites W1964757248 @default.
- W2034662724 cites W1973977373 @default.
- W2034662724 cites W1979769573 @default.
- W2034662724 cites W1985031312 @default.
- W2034662724 cites W1985952407 @default.
- W2034662724 cites W1989236130 @default.
- W2034662724 cites W1989910526 @default.
- W2034662724 cites W1990766695 @default.
- W2034662724 cites W1992635601 @default.
- W2034662724 cites W1994671833 @default.
- W2034662724 cites W1995667613 @default.
- W2034662724 cites W2000821703 @default.
- W2034662724 cites W2000878715 @default.
- W2034662724 cites W2001390446 @default.
- W2034662724 cites W2002569490 @default.
- W2034662724 cites W2012983802 @default.
- W2034662724 cites W2015529116 @default.
- W2034662724 cites W2016119283 @default.
- W2034662724 cites W2016866406 @default.
- W2034662724 cites W2021008553 @default.
- W2034662724 cites W2029695419 @default.
- W2034662724 cites W2030427115 @default.
- W2034662724 cites W2038434077 @default.
- W2034662724 cites W2043544014 @default.
- W2034662724 cites W2044669640 @default.
- W2034662724 cites W2048186190 @default.
- W2034662724 cites W2048234800 @default.
- W2034662724 cites W2048758550 @default.
- W2034662724 cites W2053265856 @default.
- W2034662724 cites W2055327934 @default.
- W2034662724 cites W2055629046 @default.
- W2034662724 cites W2056411004 @default.
- W2034662724 cites W2058924998 @default.
- W2034662724 cites W2070431442 @default.
- W2034662724 cites W2078446880 @default.
- W2034662724 cites W2080660497 @default.
- W2034662724 cites W2080927107 @default.
- W2034662724 cites W2082266584 @default.
- W2034662724 cites W2084287642 @default.
- W2034662724 cites W2088130961 @default.
- W2034662724 cites W2088847329 @default.
- W2034662724 cites W2091506494 @default.
- W2034662724 cites W2093622661 @default.
- W2034662724 cites W2095917766 @default.
- W2034662724 cites W2097957963 @default.
- W2034662724 cites W2100157321 @default.
- W2034662724 cites W2101436117 @default.
- W2034662724 cites W2101701816 @default.
- W2034662724 cites W2114553120 @default.
- W2034662724 cites W2116053549 @default.
- W2034662724 cites W2123118644 @default.
- W2034662724 cites W2123724105 @default.
- W2034662724 cites W2124922548 @default.
- W2034662724 cites W2125467645 @default.
- W2034662724 cites W2125728999 @default.
- W2034662724 cites W2125977823 @default.
- W2034662724 cites W2126409956 @default.
- W2034662724 cites W2135052708 @default.
- W2034662724 cites W2135510400 @default.
- W2034662724 cites W2136644880 @default.
- W2034662724 cites W2140887005 @default.
- W2034662724 cites W2142238829 @default.
- W2034662724 cites W2142376555 @default.
- W2034662724 cites W2143498156 @default.
- W2034662724 cites W2147417484 @default.
- W2034662724 cites W2147847259 @default.
- W2034662724 cites W2151062050 @default.
- W2034662724 cites W2155431150 @default.
- W2034662724 cites W2158227050 @default.
- W2034662724 cites W2160254914 @default.
- W2034662724 cites W2160843940 @default.
- W2034662724 cites W2163411264 @default.
- W2034662724 cites W2166365370 @default.
- W2034662724 cites W2167129914 @default.
- W2034662724 cites W2167262338 @default.
- W2034662724 cites W2168716085 @default.
- W2034662724 cites W2951554556 @default.
- W2034662724 cites W3098160327 @default.
- W2034662724 cites W3098828993 @default.
- W2034662724 cites W3099149995 @default.
- W2034662724 cites W3099490527 @default.