Star Formation Histories of Spiral Galaxies from a Multi-Wavelength Study

AbstractThe GAMA survey aims to deliver 250,000 optical spectra (3–7 Å resolution) over 250 sq. degrees to spectroscopic limits of rAB < 19.8 and KAB < 17.0 mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparable flux levels leading to a definitive multi-wavelength galaxy database. The data will be used to study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a redshift limit of z ≈ 0.4. Key science drivers include the measurement of: the halo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions; galaxy component mass-size relations; the recent merger and star-formation rates by mass, types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributions should provide individual star formation histories, ages, bulge-disc decompositions and stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subset of the sample (~ 100k) spanning both the giant and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo Australian Observatory's new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AAΩ).

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The mass dependence of star formation histories in barred spiral galaxies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stw2056 ◽

2016 ◽

Vol 463 (1) ◽

pp. 1074-1087 ◽

Cited By ~ 19

Author(s):

Christian Carles ◽

Hugo Martel ◽

Sara L. Ellison ◽

Daisuke Kawata

Keyword(s):

Star Formation ◽

Spiral Galaxies ◽

Mass Dependence ◽

Barred Spiral Galaxies ◽

Star Formation Histories

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Three-Dimensional Spectroscopy and Star Formation Histories of Field E+A Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314010515 ◽

2014 ◽

Vol 10 (S309) ◽

pp. 361-361

Author(s):

Charles T. Liu ◽

Marsha Wolf ◽

Eric J. Hooper ◽

Joshua Bather

Keyword(s):

Star Formation ◽

Three Dimensional ◽

Radio Continuum ◽

Quenching Process ◽

Multi Wavelength ◽

Star Formation Histories ◽

Initial Results ◽

Integral Field ◽

Early Type Galaxy ◽

Insight Into

AbstractWe present the initial results of an integral field spectroscopic survey of E+A galaxies in the field, which combined with radio continuum measurements and multi-wavelength photometry and imaging provides significant insight into the dynamical and star formation histories of these transitioning post-starburst systems. We focus on the E+A galaxy known as G515 (z = 0.088), a massive merger remnant that began its star formation quenching process ∼ 1.0 Gyr ago. Its relatively young stellar population contrasts with its light profile and kinematics, which are more consistent with a slowly-rotating, early-type galaxy.

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Star formation history of the galaxy merger Mrk848 with SDSS-IV MaNGA

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316008978 ◽

2016 ◽

Vol 11 (S321) ◽

pp. 304-304

Author(s):

Fang-Ting Yuan ◽

Shiyin Shen ◽

Lei Hao ◽

Maria Argudo Fernandez

Keyword(s):

Star Formation ◽

Star Formation History ◽

Galaxy Mergers ◽

The Core ◽

Integral Field Spectroscopy ◽

3D Data ◽

The Galaxy ◽

Multi Wavelength ◽

History Of ◽

Star Formation Histories

AbstractWith the 3D data of SDSS-IV MaNGA (Bundy et al. 2015) spectra and multi-wavelength SED modeling, we expect to have a better understanding of the distribution of dust, gas and star formation of galaxy mergers. For a case study of the merging galaxy Mrk848, we use both UV-to-IR broadband SED and the MaNGA integral field spectroscopy to obtain its star formation histories at the tail and core regions. From the SED fitting and full spectral fitting, we find that the star formation in the tail regions are affected by the interaction earlier than the core regions. The core regions show apparently two times of star formation and a strong burst within 500Myr, indicating the recent star formation is triggered by the interaction. The star formation histories derived from these two methods are basically consistent.

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Star Formation Histories of Massive Red Spiral Galaxies in the Local Universe

The Astrophysical Journal ◽

10.3847/1538-4357/ac06cc ◽

2021 ◽

Vol 916 (1) ◽

pp. 38

Author(s):

Shuang Zhou ◽

Cheng Li ◽

Cai-Na Hao ◽

Rui Guo ◽

Houjun Mo ◽

...

Keyword(s):

Star Formation ◽

Spiral Galaxies ◽

Local Universe ◽

Star Formation Histories

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Star Formation Histories of Spiral Galaxies from a Multi-Wavelength Study

Symposium - International Astronomical Union ◽

10.1017/s0074180900233895 ◽

1996 ◽

Vol 171 ◽

pp. 471-471

Author(s):

C. Xu

Keyword(s):

Star Formation ◽

Spiral Galaxies ◽

Star Formation Rate ◽

Formation Rate ◽

Radio Continuum ◽

Star Formation History ◽

The Past ◽

Formation History ◽

Star Formation Histories

We study the star formation histories of a sample of 113 nearby spiral galaxies using their radio continuum (20cm), FIR (40-120μm), H (1.65μm) and B (4400Å) luminosities. The first two are used as indicators of star formation rate over the past ∼ 108 years, as suggested by the tight and nearly universal FIR/radio correlation (Xu et al. 1994). Compared to other indicators of recent star formation rate such as Hα and UV, FIR and radio continuum have the advantage of being insensitive to extinction. The B luminosity is taken as star formation indicator for the time scale of 3 109 years, and the H luminosity for the time scale of 1010 years. We find: 1.The long-term star-formation history (from a few billion years to the entire Hubble time), as indicated by the B-to-H luminosity ratio, depends strongly on the Hubble type.2.The recent star-formation history in the last a few billion years, as indicated by the radio-to-B luminosity ratio and the FIR-to-B luminosity ratio, does not depend on the Hubble type.3.Galaxies of a given Hubble type have similar long-term star-formation histories. On the other hand, their recent star-formation histories in the last a few billion years can be much different: the ratio between the star-formation rate averaged over the past 108 years to that over the past 3 109 years can be different by two orders of magnitude, as indicated by the scattering of the radio-to-B luminosity ratio and that of the FIR-to-B luminosity ratio. This is not likely to be due to the extinction on the B luminosity, because the scattering of the B-to-H luminosity ratio for a given type is much smaller.

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Star formation in outer rings of S0 galaxies

Astronomy and Astrophysics ◽

10.1051/0004-6361/201834392 ◽

2018 ◽

Vol 620 ◽

pp. L7 ◽

Cited By ~ 7

Author(s):

O. Sil’chenko ◽

I. Kostiuk ◽

A. Burenkov ◽

H. Parul

Keyword(s):

Star Formation ◽

Spiral Galaxies ◽

Narrow Band ◽

Early Type ◽

Tidal Effects ◽

Ionized Gas ◽

Ring Structures ◽

Gas Accretion ◽

Star Formation Histories ◽

S0 Galaxies

Aims. Although S0 galaxies are usually thought to be “red and dead”, they often demonstrate star formation that is organized in ring structures. We try to clarify the nature of this phenomenon and its difference from star formation in spiral galaxies. Two early-type galaxies with outer rings, NGC 6534 and MCG 11-22-015, were selected to be studied. Methods. After inspecting the gas excitation in the rings using the Baldwin–Phillips–Terlevich method, we estimated the star formation rates (SFR) in the two outer rings of our galaxies using several SFR indicators derived from narrow-band photometry in the Hα emission line and archival GALEX ultraviolet images of the galaxies. Results. The ionized gas is excited by young stars in the ring of NGC 6534 and partly by shocks in MCG 11-22-015. The oxygen abundances in the HII regions of the rings are close to solar. The derived SFRs allow us to qualitatively restore star formation histories (SFH) in the rings: in NGC 6534, the SFH has been flat during the last 100–200 Myr, and in MCG 11-22-015, the star formation has started only a few Myr ago. We suggest that the rings in NGC 6534 and MCG 11-22-015 have different natures: the former is a resonant ring supplied with gas perhaps through tidal effects, and the latter has been produced by a satellite accretion. Recent outer gas accretion is implied in both cases.

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Star Formation Histories of Local Group Dwarf Galaxies

Highlights of Astronomy ◽

10.1017/s1539299600020190 ◽

1998 ◽

Vol 11 (1) ◽

pp. 125-126

Author(s):

E.K. Grebel

Keyword(s):

Star Formation ◽

Local Group ◽

Spiral Galaxies ◽

Dwarf Galaxies ◽

Close Vicinity ◽

Low Mass ◽

Star Formation Histories

The Local Group contains 37 currently known or probable member galaxies within a radius of 1.8 Mpc (Grebel 1997a). 31 of these galaxies are dwarf galaxies with MB > -17 mag. The most frequent galaxy types are low-mass, gas-poor dwarf spheroidal (dSph) galaxies, which are dominated by old and intermediate-age populations, and more massive, gas-rich dwarf irregular (dIrr) galaxies with recent star formation. DSph galaxies have been found mostly in close vicinity to the large spiral galaxies in the Local Group, while dirr galaxies tend to be more distant and isolated.

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