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 Spectral synthesis of stellar populations in the 3D era: The CALIFA experience

2014 ◽  
Vol 10 (S309) ◽  
pp. 93-98
Author(s):  
R. Cid Fernandes ◽  
E. A. D. Lacerda ◽  
R. M. González Delgado ◽  
N. Vale Asari ◽  
R. García-Benito ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Spectral Synthesis ◽  
Mass Density ◽  
Formation Rate ◽  
Stellar Populations ◽  
Data Cubes ◽  
The Mean ◽  
Stellar Masses ◽  
Star Formation Histories

AbstractMethods to recover the fossil record of galaxy evolution encoded in their optical spectra have been instrumental in processing the avalanche of data from mega-surveys along the last decade, effectively transforming observed spectra onto a long and rich list of physical properties: from stellar masses and mean ages to full star formation histories. This promoted progress in our understanding of galaxies as a whole. Yet, the lack of spatial resolution introduces undesirable aperture effects, and hampers advances on the internal physics of galaxies. This is now changing with 3D surveys. The mapping of stellar populations in data-cubes allows us to figure what comes from where, unscrambling information previously available only in integrated form. This contribution uses our starlight-based analysis of 300 CALIFA galaxies to illustrate the power of spectral synthesis applied to data-cubes. The selected results highlighted here include: (a) The evolution of the mass-metallicity and mass-density-metallicity relations, as traced by the mean stellar metallicity. (b) A comparison of star formation rates obtained from Hα to those derived from full spectral fits. (c) The relation between star formation rate and dust optical depth within galaxies, which turns out to mimic the Schmidt-Kennicutt law. (d) PCA tomography experiments.

scholarly journals Do Current X-Ray Observations Capture Most of the Black-hole Accretion at High Redshifts?

2021 ◽  
Vol 921 (2) ◽  
pp. 170
Author(s):  
Guang Yang ◽  
Vicente Estrada-Carpenter ◽  
Casey Papovich ◽  
Fabio Vito ◽  
Jonelle L. Walsh ◽  
...  
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Formation Rate ◽  
X Ray ◽  
Black Hole Accretion ◽  
Formation And Evolution ◽  
Predicted Values ◽  
Gas Accretion ◽  
Star Formation Histories ◽  
Hole Accretion

Abstract The cosmic black hole accretion density (BHAD) is critical for our understanding of the formation and evolution of supermassive black holes (BHs). However, at high redshifts (z > 3), X-ray observations report BHADs significantly (∼10 times) lower than those predicted by cosmological simulations. It is therefore paramount to constrain the high-z BHAD using independent methods other than direct X-ray detections. The recently established relation between star formation rate and BH accretion rate among bulge-dominated galaxies provides such a chance, as it enables an estimate of the BHAD from the star formation histories (SFHs) of lower-redshift objects. Using the CANDELS Lyα Emission At Reionization (CLEAR) survey, we model the SFHs for a sample of 108 bulge-dominated galaxies at z = 0.7–1.5, and further estimate the BHAD contributed by their high-z progenitors. The predicted BHAD at z ≈ 4–5 is consistent with the simulation-predicted values, but higher than the X-ray measurements (by ≈3–10 times at z = 4–5). Our result suggests that the current X-ray surveys could be missing many heavily obscured Compton-thick active galactic nuclei (AGNs) at high redshifts. However, this BHAD estimation assumes that the high-z progenitors of our z = 0.7–1.5 sample remain bulge-dominated where star formation is correlated with BH cold-gas accretion. Alternatively, our prediction could signify a stark decline in the fraction of bulges in high-z galaxies (with an associated drop in BH accretion). JWST and Origins will resolve the discrepancy between our predicted BHAD and the X-ray results by constraining Compton-thick AGN and bulge evolution at high redshifts.

scholarly journals Spatially resolved properties of galaxies with a kinematically distinct core

2021 ◽  
Vol 647 ◽  
pp. A181
Author(s):  
Kiyoaki Christopher Omori ◽  
Tsutomu T. Takeuchi
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Stellar Population ◽  
Main Body ◽  
Stellar Kinematics ◽  
Stellar Core ◽  
Spatially Resolved ◽  
Star Formation Histories ◽  
Inside Out ◽  
Detailed Picture

Aims. Interacting galaxies show unique irregularities in their kinematic structures. By investigating the spatially resolved kinematics and stellar population properties of galaxies that demonstrate irregularities, we can paint a detailed picture of the formation and evolutionary processes that took place during their lifetimes. Methods. In this work, we focused on galaxies with a specific kinematic irregularity: a kinematically distinct stellar core (KDC). In particular, we considered counter-rotating galaxies in which the core and main body of are rotating in opposite directions. We visually identified 11 MaNGA galaxies with a KDC from their stellar kinematics, and we investigated their spatially resolved stellar and gaseous kinematic properties, namely the two-dimensional stellar and gaseous velocity and velocity-dispersion (σ) maps. Additionally, we examined the stellar population properties, as well as spatially resolved recent star formation histories, using the Dn4000 and Hδ gradients. Results. The galaxies display multiple off-centred symmetrical peaks in the stellar σ maps. The gaseous velocity and σ maps display regular properties. The stellar population properties and their respective gradients show differing properties depending on the results of the spatially resolved emission line diagnostics of the galaxies, with some but not all galaxies showing inside-out quenching. The star formation histories also largely differ based on the spatially resolved emission line diagnostics, but most galaxies show indications of recent star formation either in their outskirts or core. Conclusions. We find a distinct difference in kinematic and stellar population properties in galaxies with a counter-rotating stellar core, which depends on its classification using spatially resolved emission line diagnostics.

scholarly journals THE BLACK HOLE MASSES AND STAR FORMATION RATES OFz>1 DUST OBSCURED GALAXIES: RESULTS FROM KECK OSIRIS INTEGRAL FIELD SPECTROSCOPY

2011 ◽  
Vol 141 (4) ◽  
pp. 141 ◽  
Author(s):  
J. Melbourne ◽  
Chien Y. Peng ◽  
B. T. Soifer ◽  
Tanya Urrutia ◽  
Vandana Desai ◽  
...  
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Black Hole Masses ◽  
Integral Field

scholarly journals Star Formation in Damped Lyman α Selected Galaxies

2007 ◽  
Vol 3 (S244) ◽  
pp. 284-288
Author(s):  
Lise Christensen
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
High Redshift ◽  
Neutral Hydrogen ◽  
Disk Galaxies ◽  
Local Universe ◽  
High Redshift Galaxies ◽  
Neutral Gas ◽  
Integral Field Spectroscopy ◽  
Integral Field

AbstractI present results from an ongoing survey to study galaxies associated with damped Lyman-α (DLA) systems at redshifts z>2. Integral field spectroscopy is used to search for Lyα emission line objects at the wavelengths where the emission from the quasars have been absorbed by the DLAs. The DLA galaxy candidates detected in this survey are found at distances of 10–20 kpc from the quasar line of sight, implying that galaxies are surrounded by neutral hydrogen at large distances. If we assume that the distribution of neutral gas is exponential, the scale length of the neutral gas is ~6 kpc, similar to large disk galaxies in the local Universe. The emission line luminosities imply smaller star formation rates compared to other high redshift galaxies found in luminosity selected samples.

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.

scholarly journals J-PLUS: Impact of bars on quenching timescales in nearby green valley disc galaxies

2019 ◽  
Vol 630 ◽  
pp. A88
Author(s):  
J. P. Nogueira-Cavalcante ◽  
R. Dupke ◽  
P. Coelho ◽  
M. L. L. Dantas ◽  
T. S. Gonçalves ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Clear Correlation ◽  
Spectral Indices ◽  
Local Universe ◽  
Star Forming ◽  
Magnitude Diagram ◽  
Star Formation Histories ◽  
The Impact ◽  
Disc Galaxies

Context. Between the blue cloud and the red sequence peaks on the galaxy colour–magnitude diagram there is a region sparsely populated by galaxies called the green valley. In a framework where galaxies mostly migrate on the colour–magnitude diagram from star forming to quiescent, the green valley is considered a transitional galaxy stage. The details of the processes that drive galaxies from star-forming to passive systems still remain unknown. Aims. We aim to measure the transitional timescales of nearby galaxies across the green valley, through the analysis of Galaxy Evolution Explorer and Javalambre Photometric of Local Universe Survey photometric data. Specifically, we seek to study the impact of bars on the quenching timescales. Methods. We developed a method that estimates empirically the star formation quenching timescales of green valley galaxies, assuming an exponential decay model of the star formation histories and through a combination of narrow and broad bands from the Javalambre Photometric of Local Universe Survey and Galaxy Evolution Explorer. We correlated these quenching timescales with the presence of bars. Results. We find that the Javalambre Photometric of Local Universe Survey colours F0395 −g and F0410 −g are sensitive to different star formation histories, showing, consequently, a clear correlation with the Dn(4000) and Hδ, A spectral indices. We measured quenching timescales based on these colours and we find that quenching timescales obtained with our new approach are in agreement with those determined using spectral indices. We also compared the quenching timescales of green valley disc galaxies as a function of the probability of hosting a bar. We find that galaxies with high bar probability tend to quench their star formation slowly. Conclusions. We conclude that: (1) Javalambre Photometric of Local Universe Survey filters can be used to measure quenching timescales in nearby green valley galaxies; and (2) the resulting star formation quenching timescales are longer for barred green valley galaxies. Considering that the presence of a bar indicates that more violent processes (e.g. major mergers) are absent in host galaxies, we conclude that the presence of a bar can be used as a morphological signature for slow star formation quenching.

Emission-line diagnostics of core-collapse supernova host HII regions including interacting binary population

2018 ◽  
Vol 14 (S346) ◽  
pp. 342-343
Author(s):  
Lin Xiao ◽  
J. J. Eldridge ◽  
L. Galbany ◽  
E. Stanway
Keyword(s):  
Emission Line ◽  
Spectral Synthesis ◽  
Hii Regions ◽  
Mass Gain ◽  
H Ii Regions ◽  
Type Ii ◽  
Emission Models ◽  
Distribution Type ◽  
Stellar Mergers ◽  
Integral Field

AbstractConsidering as many as 70% of massive stars interact with a binary companion (Sana et al.2012, 2014), we created a new model of the optical nebular emission of HII regions by combining the results of the Binary Population and Spectral Synthesis (BPASS, Eldridge, Stanway et al.2017) code with the photoionization code (CLOUDY). This is discussed more in detail in Xiao et al.2018a. Then we use this model to explore a variety of emission-line diagnostics of CCSN host HII regions from the PMAS/PPAK Integral-field Supernova hosts COmpilation (PISCO, Galbany et al.2018). We determine the age, metallicity and gas parameters for H II regions associated with CCSNe, contrasting the above variables to distribution type II and type Ibc SNe. We find their nebular emission and CCSN progenitor types are largely determined by past and ongoing binary interactions, for example mass loss, mass gain and stellar mergers. However we note these two types SNe have little preference in their host environment metallicity measured by oxygen abundance or in progenitor initial mass, except that at lower metallicities supernovae are more likely to be of type II. The BPASS and nebular emission models are available from bpass.auckland.ac.nz and warwick.ac.uk/bpass.

scholarly journals Imminent understanding of the structure of nearby AGN from IFUs

2013 ◽  
Vol 9 (S304) ◽  
pp. 252-252
Author(s):  
Richard Davies
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Near Infrared ◽  
Far Infrared ◽  
Absorption Lines ◽  
Robust Approach ◽  
Spatially Resolved ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

AbstractIntegral field spectroscopy provides us with immensely rich datasets about spatially resolved distributions and kinematics of emission and absorption lines. In this contribution I will describe some of the key insights that have been made about AGN using optical, near infrared, and far infrared IFUs. These encompass gas inflow and outflow mechanisms, and the relations between star formation, the torus, and accretion onto the black hole. Progress so far has largely relied on archetypal and small sets of objects. In the future, a more statistically robust approach will be required. I will end by discussing a number of issues that can easily confuse an emerging picture, and need to be borne in mind for such surveys.

scholarly journals Attenuation laws for galaxies with different star formation histories, based on the SDSS images

2009 ◽  
pp. 21-27
Author(s):  
O. Vince
Keyword(s):  
Star Formation ◽  
Sloan Digital Sky Survey ◽  
Spectral Indices ◽  
Optical Part ◽  
Sky Survey ◽  
Star Formation Histories ◽  
Attenuation Laws

Attenuation curves (laws) in the optical part of the spectrum (from about 3500 A to 9000 A) are determined for galaxies with different star formation histories (SFHs) using images in five photometrical bands from the Sloan Digital Sky Survey (SDSS). Owing to large surveys like SDSS, it is possible to define several subgroups of galaxies with similar SFHs using two spectral indices that trace SFH. Attenuation curves are analyzed in terms of SFH and compared to the curves that are often used for dust correction of the observed data. .

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