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

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.

From global to local scales in galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 391-395
Author(s):  
Sebastian F. Sánchez ◽  
Carlos Lopez Cobá
Keyword(s):  
Star Formation ◽  
Spatial Scales ◽  
Bimodal Distribution ◽  
Spectroscopic Properties ◽  
Molecular Gas ◽  
Ionized Gas ◽  
Galaxy Surveys ◽  
Quenching Process ◽  
Formation Efficiency ◽  
Integral Field

AbstractWe summarize here some of the results reviewed recently by Sanchez (2020) comprising the advances in the comprehension of galaxies in the nearby universe based on integral field spectroscopic galaxy surveys. In particular we explore the bimodal distribution of galaxies in terms of the properties of their ionized gas, showing the connection between the star-formation (quenching) process with the presence (absence) of molecular gas and the star-formation efficiency. We show two galaxy examples that illustrates the well known fact that ionization in galaxies (and the processes that produce it), does not happen monolitically at galactic scales. This highlight the importance to explore the spectroscopic properties of galaxies and the evolutionary processes unveiled by them at different spatial scales, from sub-kpc to galaxy wide.

scholarly journals Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

2021 ◽  
Vol 503 (3) ◽  
pp. 3309-3325
Author(s):  
Sabine Bellstedt ◽  
Aaron S G Robotham ◽  
Simon P Driver ◽  
Jessica E Thorne ◽  
Luke J M Davies ◽  
...  
Keyword(s):  
Star Formation ◽  
Gas Phase ◽  
Large Range ◽  
Three Dimensional ◽  
Cosmic Time ◽  
Slowing Down ◽  
History Of ◽  
Mass Assembly ◽  
Star Formation Histories ◽  
Cosmic History

ABSTRACT We analyse the metallicity histories of ∼4500 galaxies from the GAMA survey at z < 0.06 modelled by the SED-fitting code ProSpect using an evolving metallicity implementation. These metallicity histories, in combination with the associated star formation histories, allow us to analyse the inferred gas-phase mass–metallicity relation. Furthermore, we extract the mass–metallicity relation at a sequence of epochs in cosmic history, to track the evolving mass–metallicity relation with time. Through comparison with observations of gas-phase metallicity over a large range of redshifts, we show that, remarkably, our forensic SED analysis has produced an evolving mass–metallicity relationship that is consistent with observations at all epochs. We additionally analyse the three-dimensional mass–metallicity–SFR space, showing that galaxies occupy a clearly defined plane. This plane is shown to be subtly evolving, displaying an increased tilt with time caused by general enrichment, and also the slowing down of star formation with cosmic time. This evolution is most apparent at lookback times greater than 7 Gyr. The trends in metallicity recovered in this work highlight that the evolving metallicity implementation used within the SED-fitting code ProSpect produces reasonable metallicity results over the history of a galaxy. This is expected to provide a significant improvement to the accuracy of the SED-fitting outputs.

scholarly journals Comparison of stellar populations in simulated and real post-starburst galaxies in MaNGA

2020 ◽  
Vol 498 (1) ◽  
pp. 1259-1277
Author(s):  
Yirui Zheng ◽  
Vivienne Wild ◽  
Natalia Lahén ◽  
Peter H Johansson ◽  
David Law ◽  
...  
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Emission Line ◽  
Time Evolution ◽  
Spectral Synthesis ◽  
Spectral Indices ◽  
Selection Methods ◽  
Feedback Model ◽  
Star Formation Histories ◽  
Integral Field

ABSTRACT Recent integral field spectroscopic (IFS) surveys have revealed radial gradients in the optical spectral indices of post-starburst (PSB) galaxies, which can be used to constrain their formation histories. We study the spectral indices of post-processed mock IFS datacubes of binary merger simulations, carefully matched to the properties of the MaNGA IFS survey, with a variety of black hole (BH) feedback models, progenitor galaxies, orbits, and mass ratios. Based on our simulation sample, we find that only major mergers on prograde–prograde or retrograde–prograde orbits in combination with a mechanical BH feedback model can form galaxies with weak enough ongoing star formation, and therefore absent H α emission, to be selected by traditional PSB selection methods. We find strong fluctuations in nebular emission line strengths, even within the PSB phase, suggesting that H α selected PSBs are only a subsample of the underlying population. The global PSB population can be more robustly identified using stellar continuum-based approaches. The difficulty in reproducing the very young PSBs in simulations potentially indicates that new sub-resolution star formation recipes are required to properly model the process of star formation quenching. In our simulations, we find that the starburst peaks at the same time at all radii, but is stronger and more prolonged in the inner regions. This results in a strong time evolution in the radial gradients of the spectral indices that can be used to estimate the age of the starburst without reliance on detailed star formation histories from spectral synthesis models.

scholarly journals CORNISH: A 5 GHz VLA survey of the Galactic plane

2009 ◽  
Vol 5 (H15) ◽  
pp. 781-781
Author(s):  
Cormac R. Purcell ◽  
Melvin G. Hoare ◽  
Keyword(s):  
Star Formation ◽  
Galactic Plane ◽  
Radio Continuum ◽  
High Mass ◽  
Mass Star ◽  
Multi Wavelength ◽  
Region 10 ◽  
5 Ghz ◽  
Infrared Survey ◽  
Key Questions

AbstractThe CORNISH (Co-Ordinated Radio ‘N’ Infrared Survey for High-mass star formation) project is the radio continuum part of a series of multi-wavelength surveys of the Galactic Plane that focus on the northern GLIMPSE-I region (10° < l <65°, |b| < 1°) observed by the SPITZER satellite in the mid-infrared (Churchwell et al. 2009). CORNISH has delivered a complementary 5 GHz arcsecond resolution, radio-continuum survey to address key questions in high-mass star formation as well as many other areas of astrophysics.

scholarly journals Galaxy And Mass Assembly (GAMA)

2008 ◽  
Vol 4 (S254) ◽  
pp. 469-474
Author(s):  
Simon P. Driver ◽  
Keyword(s):  
Star Formation ◽  
Dwarf Galaxy ◽  
Mass Function ◽  
Dual Beam ◽  
Individual Star ◽  
Multi Wavelength ◽  
Mass Assembly ◽  
Galaxy Populations ◽  
Star Formation Histories ◽  
Baryonic Mass

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).

scholarly journals Optical SED models of galaxy mergers

2011 ◽  
Vol 7 (S284) ◽  
pp. 193-197
Author(s):  
Gregory F. Snyder ◽  
T. J. Cox ◽  
Christopher C. Hayward ◽  
Lars Hernquist ◽  
Patrik Jonsson
Keyword(s):  
Three Dimensional ◽  
Interacting Galaxies ◽  
Galaxy Mergers ◽  
Hydrodynamic Simulations ◽  
Spatially Resolved ◽  
Multi Wavelength ◽  
Field Unit ◽  
Effects Of Feedback ◽  
Dust Attenuation ◽  
Integral Field

AbstractI discuss recent work in which we construct models of poststarburst galaxies by combining fully three-dimensional hydrodynamic simulations of galaxy mergers with radiative transfer calculations of dust attenuation. The poststarburst signatures can occur shortly after a bright starburst phase in gas-rich mergers, and thus offer a unique opportunity to study the formation of bulges and the effects of feedback. Several additional applications of spatially-resolved spectroscopic models of interacting galaxies include multi-wavelength studies of AGN/starburst diagnostics, mock integral field unit data to interpret the evolution of ULIRGs, and the ‘Green Valley’.Optical spectra of simulated major gas-rich galaxy mergers can be found at http://www.cfa.harvard.edu/~gsnyder

scholarly journals Understanding galaxy mergers and AGN feedback with UVIT

2019 ◽  
Vol 15 (S356) ◽  
pp. 345-347
Author(s):  
Khatun Rubinur ◽  
Mousumi Das ◽  
Preeti Kharb ◽  
P. T. Rahne
Keyword(s):  
Star Formation ◽  
Pilot Study ◽  
Active Galactic Nuclei ◽  
Negative Feedback ◽  
Galactic Nuclei ◽  
Galaxy Mergers ◽  
Imaging Telescope ◽  
Multi Wavelength ◽  
Initial Results

AbstractSimulations expect an enhanced star-formation and active galactic nuclei (AGN) activity during galaxy mergers, which can lead to formation of binary/dual AGN. AGN feedback can enhance or suppress star-formation. We have carried out a pilot study of a sample of ˜10 dual nuclei galaxies with AstroSat’s Ultraviolet Imaging Telescope (UVIT). Here, we present the initial results for two sample galaxies (Mrk 739, ESO 509) and deep multi-wavelength data of another galaxy (Mrk 212). UVIT observations have revealed signatures of positive AGN feedback in Mrk 739 and Mrk 212, and negative feedback in ESO 509. Deeper UVIT observations have recently been approved; these will provide better constraints on star-formation as well as AGN feedback in these systems.

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

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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