The Faint End of the Centaurus A Satellite Luminosity Function
Name:
Crnojević_2019_ApJ_872_80.pdf
Size:
3.438Mb
Format:
PDF
Description:
Final Published version
Affiliation
Univ Arizona, Steward ObservUniv Arizona, Dept Astron
Issue Date
2019-02-10Keywords
galaxies: dwarfgalaxies: evolution
galaxies: groups: individual (Cen A)
galaxies: halos
galaxies: luminosity function, mass function
galaxies: photometry
Metadata
Show full item recordPublisher
IOP PUBLISHING LTDCitation
D. Crnojević et al 2019 ApJ 872 80Journal
ASTROPHYSICAL JOURNALRights
© 2019. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
The Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS) is constructing a wide-field map of the resolved stellar populations in the extended halos of these two nearby, prominent galaxies. We present new Magellan/Megacam imaging of a similar to 3 deg(2) area around Centaurus A (Cen A), which filled in much of our coverage to its south, leaving a nearly complete halo map out to a projected radius of similar to 150 kpc and allowing us to identify two new resolved dwarf galaxies. We have additionally obtained deep Hubble Space Telescope (HST) optical imaging of 11 out of the 13 candidate dwarf galaxies identified around Cen A and presented in Crnojevic et al. 2016a: seven are confirmed to be satellites of Cen A, while four are found to be background galaxies. We derive accurate distances, structural parameters, luminosities, and photometric metallicities for the seven candidates confirmed by our HST/ACS imaging. We further study the stellar population along the similar to 60 kpc long (in projection) stream associated with Dw3, which likely had an initial brightness of M-V similar to -15 and shows evidence for a metallicity gradient along its length. Using the total sample of 11 dwarf satellites discovered by the PISCeS survey, as well as 13 brighter previously known satellites of Cen A, we present a revised galaxy luminosity function for the Cen A group down to a limiting magnitude of M-V similar to -8, which has a slope of -1.14 +/- 0.17, comparable to that seen in the Local Group and in other nearby groups of galaxies.ISSN
1538-4357Version
Final published versionSponsors
NASA from the Space Telescope Science Institute [NNX14AF84G, HST-GO-13856.001]; NSF [AST-1514763, AST-1814208, AST-1821967, AST-1821987, AST-1813708, AST-1813466, AST-1010039, AST-1412504, AST-1412792]; Packard Fellowship; Natural Sciences and Engineering Research Council of Canada (NSERC); National Science Foundation [PHYS-1066293]; Aspen Center for Physics; Smithsonian Astrophysical Observatory; NASA [NNX14AF84G, NAS 5-26555]Additional Links
http://stacks.iop.org/0004-637X/872/i=1/a=80?key=crossref.ee71687c6486f768c1653583d2bfb604Scopus Count
Collections
Related items
Showing items related by title, author, creator and subject.
-
The Massive and Distant Clusters of WISE Survey. V. Extended Radio Sources in Massive Galaxy Clusters at z ∼ 1We present the results from a pilot study with the Karl G. Jansky Very Large Array to determine the radio morphologies of extended radio sources and the properties of their host-galaxies in 10 massive galaxy clusters at z similar to 1, an epoch in which clusters are assembling rapidly. These clusters are drawn from a parent sample of WISE-elected galaxy clusters that were cross-correlated with the VLA Faint Images of the Radio Sky at Twenty-Centimeters survey to identify extended radio sources within 1' of the cluster centers. Out of the 10 targeted sources, 6 are FR II sources, 1 is an FR I source, and 3 have undetermined morphologies. Eight radio sources have associated Spitzer data, 75% presenting infrared counterparts. A majority of these counterparts are consistent with being massive galaxies. The angular extent of the FR sources exhibits a strong correlation with the cluster-centric radius, which warrants further investigation with a larger sample.
-
Nuclear starburst activity induced by elongated bulges in spiral galaxiesWe study the effects of bulge elongation on the star formation activity in the centres of spiral galaxies using the data from the Sloan Digital Sky Survey Data Release 7. We construct a volume-limited sample of face-on spiral galaxies with Mr < −19.5 mag at 0.02 ≤ z < 0.055 by excluding barred galaxies, where the aperture of the SDSS spectroscopic fibre covers the bulges of the galaxies. We adopt the ellipticity of bulges measured by Simard et al., who performed two-dimensional bulge + disc decompositions using the SDSS images of galaxies, and identify nuclear starbursts using the fibre specific star formation rates derived from the SDSS spectra. We find a statistically significant correlation between bulge elongation and nuclear starbursts in the sense that the fraction of nuclear starbursts increases with bulge elongation. This correlation is more prominent for fainter and redder galaxies, which exhibit higher ratios of elongated bulges. We find no significant environmental dependence of the correlation between bulge elongation and nuclear starbursts. These results suggest that non-axisymmetric bulges can efficiently feed the gas into the centre of galaxies to trigger nuclear starburst activity.
-
Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steelObservational systematics complicate comparisons with theoretical models limiting understanding of galaxy evolution. In particular, different empirical determinations of the stellar mass function imply distinct mappings between the galaxy and halo masses, leading to diverse galaxy evolutionary tracks. Using our state-of-the-art STatistical sEmi-Empirical modeL, STEEL, we show fully self-consistent models capable of generating galaxy growth histories that simultaneously and closely agree with the latest data on satellite richness and star formation rates at multiple redshifts and environments. Central galaxy histories are generated using the central halo mass tracks from state-of-the-art statistical dark matter accretion histories coupled to abundance matching routines. We show that too flat high-mass slopes in the input stellar mass-halo mass relations as predicted by previous works, imply non-physical stellar mass growth histories weaker than those implied by satellite accretion alone. Our best-fitting models reproduce the satellite distributions at the largest masses and highest redshifts probed, the latest data on star formation rates and its bimodality in the local Universe, and the correct fraction of ellipticals. Our results are important to predict robust and self-consistent stellar mass-halo mass relations and to generate reliable galaxy mock catalogues for the next generations of extragalactic surveys such as Euclid and LSST.
