FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2029890567> ?p ?o ?g. }

• W2029890567 endingPage "3141" @default.
• W2029890567 startingPage "3128" @default.
• W2029890567 abstract "We use a sample of 9397 low-redshift (z ≤ 0.1) galaxies with a close companion to investigate the connection between mergers and luminous infrared (IR) galaxies (LIRGs). The pairs are selected from the Sloan Digital Sky Survey (SDSS) and have projected separations rp ≤ 80 h|${^{- 1}_{70}}$| kpc, relative velocities ΔV ≤ 300 km s−1 and stellar mass ratios within a factor of 1:10. A control sample consisting of four galaxies per pair galaxy is constructed by simultaneously matching in stellar mass, redshift and environment to galaxies with no close companion. The IR luminosities (LIR) of galaxies in the pair and control samples are determined from the SDSS – Infrared Astronomical Satellite (IRAS) matched catalogue of Hwang et al. Over the redshift range of our pairs sample, the IRAS matches are complete to LIRG luminosities (LIR ≥ 1011 L⊙), allowing us to investigate the connection between mergers and luminous IR galaxies. We find a trend for increasing LIRG fraction towards smaller pair separations, peaking at a factor of ∼5–10 above the median control fraction at the smallest separations (rp < 20 h|${^{- 1}_{70}}$| kpc), but remaining elevated by a factor ∼2–3 even out to 80 h|${^{- 1}_{70}}$| kpc (the widest separations in our sample). LIRG pairs predominantly have high star formation rates (SFRs), high extinction and are found in relatively low-density environments, relative to the full pairs sample. We also find that LIRGs are most likely to be found in high-mass galaxies which have an approximately equal-mass companion. We confirm the results of previous studies that both the active galactic nucleus (AGN) fraction and merger fraction increase strongly as a function of IR luminosity. About 7 per cent of LIRGs are associated with major mergers, as defined within the criteria and mass completion of our sample. Finally, we quantify an SFR offset (ΔSFR) as the enhancement (or decrement) relative to star-forming galaxies of the same mass and redshift. We demonstrate that there is a clear connection between the ΔSFR and the classification of a galaxy as a LIRG that is mass dependent. Most of the LIRGs in our merger sample are relatively high-mass galaxies (log (M⋆/M⊙) > 10.5), likely because the SFR enhancement required to produce LIRG luminosities is more modest than at low masses. The ΔSFR offers a redshift-independent metric for the identification of the galaxies with the most enhanced star-forming rates that does not rely on fixed LIR boundaries." @default.
• W2029890567 created "2016-06-24" @default.
• W2029890567 creator A5008219850 @default.
• W2029890567 creator A5042374450 @default.
• W2029890567 creator A5044000422 @default.
• W2029890567 creator A5052707747 @default.
• W2029890567 creator A5077848676 @default.
• W2029890567 date "2013-02-19" @default.
• W2029890567 modified "2023-09-27" @default.
• W2029890567 title "Galaxy pairs in the Sloan Digital Sky Survey – VII. The merger–luminous infrared galaxy connection" @default.
• W2029890567 cites W1760966995 @default.
• W2029890567 cites W1946092078 @default.
• W2029890567 cites W1960407247 @default.
• W2029890567 cites W1966308739 @default.
• W2029890567 cites W1966497244 @default.
• W2029890567 cites W1973275093 @default.
• W2029890567 cites W1973637537 @default.
• W2029890567 cites W1982717117 @default.
• W2029890567 cites W1985952407 @default.
• W2029890567 cites W1989738732 @default.
• W2029890567 cites W1989910526 @default.
• W2029890567 cites W1993355650 @default.
• W2029890567 cites W1994968723 @default.
• W2029890567 cites W1997559701 @default.
• W2029890567 cites W1997662069 @default.
• W2029890567 cites W2007608095 @default.
• W2029890567 cites W2009140128 @default.
• W2029890567 cites W2009721953 @default.
• W2029890567 cites W2011193914 @default.
• W2029890567 cites W2014595241 @default.
• W2029890567 cites W2016328704 @default.
• W2029890567 cites W2025629511 @default.
• W2029890567 cites W2029634641 @default.
• W2029890567 cites W2031203855 @default.
• W2029890567 cites W2032020213 @default.
• W2029890567 cites W2033648059 @default.
• W2029890567 cites W2036491734 @default.
• W2029890567 cites W2037136553 @default.
• W2029890567 cites W2047688075 @default.
• W2029890567 cites W2049698250 @default.
• W2029890567 cites W2051128239 @default.
• W2029890567 cites W2054026519 @default.
• W2029890567 cites W2055137814 @default.
• W2029890567 cites W2057939717 @default.
• W2029890567 cites W2061140827 @default.
• W2029890567 cites W2065975941 @default.
• W2029890567 cites W2068577843 @default.
• W2029890567 cites W2069847092 @default.
• W2029890567 cites W2074312913 @default.
• W2029890567 cites W2091010926 @default.
• W2029890567 cites W2096842323 @default.
• W2029890567 cites W2097351307 @default.
• W2029890567 cites W2099195140 @default.
• W2029890567 cites W2106879059 @default.
• W2029890567 cites W2109472987 @default.
• W2029890567 cites W2111695089 @default.
• W2029890567 cites W2112193291 @default.
• W2029890567 cites W2114553120 @default.
• W2029890567 cites W2115019311 @default.
• W2029890567 cites W2120422993 @default.
• W2029890567 cites W2121584184 @default.
• W2029890567 cites W2123267088 @default.
• W2029890567 cites W2125977823 @default.
• W2029890567 cites W2135632948 @default.
• W2029890567 cites W2137064512 @default.
• W2029890567 cites W2147847259 @default.
• W2029890567 cites W2150995848 @default.
• W2029890567 cites W2153140383 @default.
• W2029890567 cites W2156657195 @default.
• W2029890567 cites W2158486245 @default.
• W2029890567 cites W2161190330 @default.
• W2029890567 cites W2163212281 @default.
• W2029890567 cites W2166365370 @default.
• W2029890567 cites W2168495929 @default.
• W2029890567 cites W2600822636 @default.
• W2029890567 cites W2761193714 @default.
• W2029890567 cites W2949884473 @default.
• W2029890567 cites W2951432302 @default.
• W2029890567 cites W3098017933 @default.
• W2029890567 cites W3098784892 @default.
• W2029890567 cites W3098801730 @default.
• W2029890567 cites W3098891757 @default.
• W2029890567 cites W3099149995 @default.
• W2029890567 cites W3099229315 @default.
• W2029890567 cites W3099664213 @default.
• W2029890567 cites W3099677729 @default.
• W2029890567 cites W3100302622 @default.
• W2029890567 cites W3101085923 @default.
• W2029890567 cites W3101352865 @default.
• W2029890567 cites W3101767981 @default.
• W2029890567 cites W3102818270 @default.
• W2029890567 cites W3103138185 @default.
• W2029890567 cites W3103868583 @default.
• W2029890567 cites W3103994273 @default.
• W2029890567 cites W3104119696 @default.
• W2029890567 cites W3105028954 @default.
• W2029890567 cites W3106285913 @default.
• W2029890567 cites W3106474653 @default.

• next