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Galaxy And Mass Assembly (GAMA): galaxy close pairs, mergers and the future fate of stellar mass

Hopkins AM; Lara-Lopez MA; Mahajan S; Moffett A; Prescott M; Robotham ASG; Obreschkow D; Liske J; Taylor EN; Cluver M; Bauer AE; Lopez-Sanchez AR; Holwerda BW; Driver SP; Penny SJ; Drinkwater MJ; Bland-Hawthorn J; Wilkins SM; Loveday J; Norberg P; Kelvin LS; Owers MS; Davies LJM; Pimbblet K; Baldry IK; Brough S; De Propris R; van Kampen E; Brown MJI; Agius NK; McNaught-Roberts T

Galaxy And Mass Assembly (GAMA): galaxy close pairs, mergers and the future fate of stellar mass

Hopkins AM
Lara-Lopez MA
Mahajan S
Moffett A
Prescott M
Robotham ASG
Obreschkow D
Liske J
Taylor EN
Cluver M
Bauer AE
Lopez-Sanchez AR
Holwerda BW
Driver SP
Penny SJ
Drinkwater MJ
Bland-Hawthorn J
Wilkins SM
Loveday J
Norberg P
Kelvin LS
Owers MS
Davies LJM
Pimbblet K
Baldry IK
Brough S
De Propris R
van Kampen E
Brown MJI
Agius NK
McNaught-Roberts T
Katso/Avaa
This article has been accepted for publication in Monthly notices ©: 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. (3.592Mb)
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OXFORD UNIV PRESS
doi:10.1093/mnras/stu1604
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Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042715468
Tiivistelmä


We use a highly complete subset of the Galaxy And Mass Assembly II (GAMA-II) redshift sample to fully describe the stellar mass dependence of close pairs and mergers between 10(8) and 10(12)M(circle dot). Using the analytic form of this fit we investigate the total stellar mass accreting on to more massive galaxies across all mass ratios. Depending on how conservatively we select our robust merging systems, the fraction of mass merging on to more massive companions is 2.0-5.6 per cent. Using the GAMA-II data we see no significant evidence for a change in the close pair fraction between redshift z = 0.05 and 0.2. However, we find a systematically higher fraction of galaxies in similar mass close pairs compared to published results over a similar redshift baseline. Using a compendium of data and the function gamma(M) = A(1 + z)(m) to predict the major close pair fraction, we find fitting parameters of A = 0.021 +/- 0.001 and m = 1.53 +/- 0.08, which represents a higher low-redshift normalization and shallower power-law slope than recent literature values. We find that the relative importance of in situ star formation versus galaxy merging is inversely correlated, with star formation dominating the addition of stellar material below M* and merger accretion events dominating beyond M*. We find mergers have a measurable impact on the whole extent of the galaxy stellar mass function (GSMF), manifest as a deepening of the 'dip' in the GSMF over the next similar to Gyr and an increase in M* by as much as 0.01-0.05 dex.

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