Multicolor photoelectric photometry of bright galaxies. 11

Tifft, W. G.

doi:10.1086/108979

Cited by 20 publications

(6 citation statements)

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“…Despite these differences, the IFU-based results obtained so far are all consistent with the "inside-out" growth of galactic disks (White & Frenk 1991;Mo et al 1998), a picture that was supported previously by both numerical simulations (e.g. Brook et al 2006) and abundant studies of broadband color gradients pioneered more than 50 years ago by Tifft (1963).…”

Section: D Maps and Radial Profilessupporting

confidence: 77%

P-MaNGA: GRADIENTS IN RECENT STAR FORMATION HISTORIES AS DIAGNOSTICS FOR GALAXY GROWTH AND DEATH

Wang

Lin

et al. 2015

ApJ

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We present an analysis of the data produced by the MaNGA prototype run (P-MaNGA), aiming to test how the radial gradients in recent star formation histories, as indicated by the 4000Å-break (D n (4000)), Hδ absorption (EW(Hδ A )) and Hα emission (EW(Hα)) indices, can be useful for understanding disk growth and star formation cessation in local galaxies. We classify 12 galaxies observed on two P-MaNGA plates as either centrally quiescent (CQ) or centrally star-forming (CSF), according to whether D n (4000) measured in the central spaxel of each datacube exceeds 1.6. For each spaxel we generate both 2D maps and radial profiles of D n (4000), EW(Hδ A ) and EW(Hα). We find that CSF galaxies generally show very weak or no radial variation in these diagnostics. In contrast, CQ galaxies present significant radial gradients, in the sense that D n (4000) decreases, while both EW(Hδ A ) and EW(Hα) increase from the galactic center outward. The outer regions of the galaxies show greater scatter on diagrams relating the three parameters than their central parts. In particular, the clear separation between centrally-measured quiescent and star-forming galaxies in these diagnostic planes is largely filled in by the outer parts of galaxies whose global colors place them in the green valley, supporting the idea that the green valley represents a transition between blue-cloud and red-sequence phases, at least in our small sample. These results are consistent with a picture in which the cessation of star formation propagates from the center of a galaxy outwards as it moves to the red sequence.

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Section: D Maps and Radial Profilessupporting

confidence: 77%

P-MaNGA: GRADIENTS IN RECENT STAR FORMATION HISTORIES AS DIAGNOSTICS FOR GALAXY GROWTH AND DEATH

Wang

Lin

et al. 2015

ApJ

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“…The existence of colour gradients in both spiral and elliptical galaxies has been known for more than 50 years (e.g. Tifft 1963). In the 1970's, astronomers began to image galaxies at near-IR wavelengths for the first time.…”

Section: Colour Profiles Of Spiral and Elliptical Galaxies: Backgroundmentioning

confidence: 99%

The outer stellar populations and environments of unusually H i-rich galaxies

Kauffmann

2015

Monthly Notices of the Royal Astronomical Society

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We investigate the nature of HI-rich galaxies from the ALFALFA and GASS surveys, which are defined as galaxies in the top 10th percentile in atomic gas fraction at a given stellar mass. We analyze outer (R > 1.5R e ) stellar populations for a subset of face-on systems using optical g − r versus r − z colour/colour diagrams. The results are compared with those from control samples that are defined without regard to atomic gas content, but are matched in redshift, stellar mass and structural parameters. HIrich early-type (C > 2.6) and late-type (C < 2.6) galaxies are studied separately. When compared to the control sample, the outer stellar populations of the majority of HI-rich early-type galaxies are shifted in the colour/colour plane along a locus consistent with younger stellar ages, but similar metallicities. The outer colours of HI-rich late-type galaxies are much bluer in r − z than the HI-rich early types, and we infer that they have outer disks which are both younger and more metal-poor. We then proceed to analyze the galaxy environments of HI-rich galaxies on scales comparable to the expected virial radii of their dark matter halos (R < 500 kpc). Low mass (log M * < 10.5) HI-rich early-type galaxies have galaxy environments that differ significantly from the control sample. HI-rich early types are more likely to be central rather than satellite systems. Their satellites are also less massive and have younger stellar populations. Similar, but weaker effects are found for HI-rich late-type galaxies of the same mass. In addition, we find that the satellites of HI-rich late-types exhibit a greater tendency to align along the major axis of the primary. No environmental differences are found for massive (log M * > 10.5) HI-rich galaxies, regardless of type.We then undertook a follow-up program to map the HI in a small sample of 25 unusually HI-rich galaxies and 25 "control" galaxies with normal HI content using the Westerbork Synthesis Radio Telescope (WSRT; Wang et al 2013, c 0000 RAS

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“…Early attempts to study the stellar content of early-type galaxies were based on colours from wide and narrow band photometry (Baum 1959;Tifft 1963;Wood 1966;McClure & van den Bergh 1968;Faber 1973) and on empirical synthesis of the populations using the observed colours of nearby early-types as basis. These early methods can be considered as the pioneers of the current photo-spectral fitting techniques, which are the main topic of the present paper.…”

Section: Introductionmentioning

confidence: 99%

Stellar populations of galaxies in the ALHAMBRA survey up toz ~ 1

Díaz-García

Cenarro

López-Sanjuan

et al. 2015

A&A

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Aims. We present MUFFIT, a new generic code optimized to retrieve the main stellar population parameters of galaxies in photometric multi-filter surveys, and check its reliability and feasibility with real galaxy data from the ALHAMBRA survey. Methods. Making use of an error-weighted χ 2 -test, we compare the multi-filter fluxes of galaxies with the synthetic photometry of mixtures of two single stellar populations at different redshifts and extinctions, to provide the most likely range of stellar population parameters (mainly ages and metallicities), extinctions, redshifts, and stellar masses. To improve the diagnostic reliability, MUFFIT identifies and removes from the analysis those bands that are significantly affected by emission lines. The final parameters and their uncertainties are derived by a Monte Carlo method, using the individual photometric uncertainties in each band. Finally, we discuss the accuracies, degeneracies, and reliability of MUFFIT using both simulated and real galaxies from ALHAMBRA, comparing with results from the literature. Results. MUFFIT is a precise and reliable code to derive stellar population parameters of galaxies in ALHAMBRA. Using the results from photometric-redshift codes as input, MUFFIT improves the photometric-redshift accuracy by ∼10-20%. MUFFIT also detects nebular emissions in galaxies, providing physical information about their strengths. The stellar masses derived from MUFFIT show excellent agreement with the COSMOS and SDSS values. In addition, the retrieved age-metallicity locus for a sample of z ≤ 0.22 early-type galaxies in ALHAMBRA at different stellar mass bins are in very good agreement with the ones from SDSS spectroscopic diagnostics. Moreover, a one-to-one comparison between the redshifts, ages, metallicities, and stellar masses derived spectroscopically for SDSS and by MUFFIT for ALHAMBRA reveals good qualitative agreements in all the parameters, hence reinforcing the strengths of multi-filter galaxy data and optimized analysis techniques, like MUFFIT, to conduct reliable stellar population studies.

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Multicolor photoelectric photometry of bright galaxies. 11

Cited by 20 publications

References 0 publications

P-MaNGA: GRADIENTS IN RECENT STAR FORMATION HISTORIES AS DIAGNOSTICS FOR GALAXY GROWTH AND DEATH

P-MaNGA: GRADIENTS IN RECENT STAR FORMATION HISTORIES AS DIAGNOSTICS FOR GALAXY GROWTH AND DEATH

The outer stellar populations and environments of unusually H i-rich galaxies

Stellar populations of galaxies in the ALHAMBRA survey up toz ~ 1

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