J/MNRAS/433/2986 SDSSRC3 sample morphological classifications (Wilman+, 2013)
The hierarchical origins of observed galaxy morphology.
Wilman D.J., Fontanot F., De Lucia G., Erwin P., Monaco P.
<Mon. Not. R. Astron. Soc., 433, 2986-3004 (2013)>
=2013MNRAS.433.2986W 2013MNRAS.433.2986W
ADC_Keywords: Galaxy catalogs ; Morphology
Keywords: galaxies: bulges - galaxies: elliptical and lenticular, cD -
galaxies: haloes - galaxies: star formation - galaxies: statistics -
galaxies: structure
Abstract:
Galaxies grow primarily via accretion-driven star formation in discs
and merger-driven growth of bulges. These processes are implicit in
semi-analytical models of galaxy formation, with bulge growth in
particular relating directly to the hierarchical build-up of haloes
and their galaxies. In this paper, we consider several implementations
of two semi-analytical models. Focusing on implementations in which
bulges are formed during mergers only, we examine the fractions of
elliptical galaxies and both passive and star-forming disc galaxies as
functions of stellar and halo mass, for central and satellite systems.
This is compared to an observational cross-matched Sloan Digital Sky
Survey+Third Reference Catalog of Bright Galaxies z∼0 sample of
galaxies with accurate visual morphological classifications and
M*>1010.5M☉. The models qualitatively reproduce the observed
increase of elliptical fraction with stellar mass, and with halo mass
for central galaxies, supporting the idea that observed ellipticals
form during major mergers. However, the overall elliptical fraction
produced by the models is much too high compared with the z∼0 data.
Since the 'passive' - i.e. non-star-forming - fractions are
approximately reproduced, and since the fraction which are
star-forming disc galaxies is also reproduced, the problem is that the
models overproduce ellipticals at the expense of passive S0 and spiral
galaxies. Bulge growth implementations (tuned to reproduce
simulations) which allow the survival of residual discs in major
mergers still destroy too much of the disc. Increasing the lifetime of
satellites, or allowing significant disc regrowth around merger
remnants, merely increases the fraction of star-forming disc galaxies.
Instead, it seems necessary to reduce the mass ratios of merging
galaxies, so that most mergers produce modest bulge growth in disc
galaxy remnants instead of ellipticals. This could be a natural
consequence of tidal stripping of stars from infalling satellite
galaxies, a process not considered in our models. However, a high
efficiency of quenching during and/or subsequent to minor mergers is
still required to keep the passive fraction high.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 854 The SDSSRC3 sample morphological classifications
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See also:
VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Galaxy name
15- 24 F10.6 deg RAdeg SDSS-DR4 Right ascension (J2000)
26- 35 F10.6 deg DEdeg SDSS-DR4 Declination (J2000)
37- 42 F6.4 --- z SDSS-DR4 Redshift
44- 48 F5.2 [Msun] logM* Stellar mass (1)
51- 57 A7 --- MT-RC3 RC3 morphological type (VII/155)
62- 68 A7 --- MType Revised morphological type based on WE12 (2)
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Note (1): computed using the SDSS photometry and the colour-based M/L ratios
of Zibetti et al. (2009MNRAS.400.1181Z 2009MNRAS.400.1181Z) (see the text).
Note (2): The WE12 (Wilman & Erwin, 2012ApJ...746..160W 2012ApJ...746..160W) morphologies are the
same as in RC3 (Cat. VII/155) except where we have reclassified galaxies
(or provided classifications where none existed).
If we revised an RC3 disc classification (e.g., S0 to spiral), we retained
any additional morphological information (rings, etc.) as in RC3.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Jul-2014