2018MNRAS.480.2236A


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.29CET06:50:06

2018MNRAS.480.2236A - Mon. Not. R. Astron. Soc., 480, 2236-2246 (2018/October-3)

The rise and fall of the UV upturn: z = 0.3, 0.55, and 0.7.

ALI S.S., BREMER M.N., PHILLIPPS S. and DE PROPRIS R.

Abstract (from CDS):

We have analysed the strength of the ultraviolet (UV) upturn in red sequence galaxies with luminosities reaching to below the L* point within four clusters at z = 0.3, 0.55, and 0.7. We find that the incidence and strength of the upturn remains constant up to z = 0.55. In comparison, the prevalence and strength of the UV upturn is significantly diminished in the z = 0.7 cluster, implying that the stellar population responsible for the upturn in a typical red sequence galaxy is only just developing at this redshift and is essentially fully developed by ∼1 Gyr later. Of all the mainstream models that seek to explain the UV upturn phenomenon, it is those that generate the upturn through the presence of a Helium-enhanced stellar sub-population on the (hot) horizontal branch that are most consistent with this behaviour. The epoch (z = 0.7) where the stars responsible for the upturn first evolve from the red giant branch places constraints on their age and chemical abundances. By comparing our results with the prediction made by the YEPS Helium-enhanced spectrophotometic models, we find that a solar metallicity sub-population that displays a consistent upturn between 0 < z < 0.55 but then fades by z = 0.7 would require a Helium abundance of Y >= 0.45, if formed at zf ∼ 4. Later formation redshifts and/or higher metallicity would further increase the Helium enhancement required to produce the observed upturn in these clusters and vice versa.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: horizontal branch - galaxies: clusters: individual - galaxies: evolution - galaxies: formation

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ACO 2744 ClG 00 14 20.03 -30 23 17.8           ~ 546 0
2 M 32 IG 00 42 41.825 +40 51 54.61 9.51 9.03 8.08     ~ 1982 2
3 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10680 1
4 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 1904 1
5 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1503 0
6 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 334 0
7 IRAS 09110-6439 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1213 0
8 ClG J1004+4112 ClG 10 04 34.180 +41 12 43.50           ~ 38 3
9 MCS J1149.5+2223 ClG 11 49 35.8 +22 23 55           ~ 297 0
10 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5705 0
11 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6085 3
12 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4134 2
13 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1007 0
14 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 2940 0
15 NGC 6388 GlC 17 36 17.461 -44 44 08.34   7.40       ~ 781 1
16 NGC 6441 GlC 17 50 13.06 -37 03 05.2   9.26 8.00     ~ 749 0

    Equat.    Gal    SGal    Ecl

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2020.01.29-06:50:06

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