scholarly journals Compact Binaries as Tracers of Star Formation Histories: the XMM Survey of M31

1999 ◽  
Vol 192 ◽  
pp. 496-502
Author(s):  
U. Kolb ◽  
J. Osborne ◽  
M. G. Watson
Keyword(s):  
Star Formation ◽  
Evolutionary History ◽  
Star Formation History ◽  
X Ray ◽  
Compact Binaries ◽  
Normal Galaxies ◽  
Formation History ◽  
History Of ◽  
Star Formation Histories ◽  
X Ray Binaries

X-ray binaries (XBs) dominate the X-ray emission of normal galaxies. The new X-ray satellite XMM will study the XB population of M31 in detail. The resulting M31 sample will significantly advance our understanding of the evolutionary history of XBs, and ultimately allow us to probe the star formation history of stellar populations by X-ray observations.

scholarly journals Be X-ray binaries in the SMC as indicators of mass-transfer efficiency

2020 ◽  
Vol 498 (4) ◽  
pp. 4705-4720 ◽  
Author(s):  
Serena Vinciguerra ◽  
Coenraad J Neijssel ◽  
Alejandro Vigna-Gómez ◽  
Ilya Mandel ◽  
Philipp Podsiadlowski ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Star Formation ◽  
Compact Object ◽  
Star Formation History ◽  
Be Stars ◽  
X Ray ◽  
Formation History ◽  
History Of ◽  
Minimal Mass ◽  
X Ray Binaries

ABSTRACT Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the compas population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stable mass transfer, their mass distribution suggests that at least $\sim 30{{\ \rm per\ cent}}$ of the mass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy’s burst of star formation ∼20–40 Myr ago.

scholarly journals Spatial variations in the star formation history of the Large Magellanic Cloud

2008 ◽  
Vol 4 (S256) ◽  
pp. 281-286
Author(s):  
Carme Gallart ◽  
Ingrid Meschin ◽  
Antonio Aparicio ◽  
Peter B. Stetson ◽  
Sebastián L. Hidalgo
Keyword(s):  
Star Formation ◽  
Outer Part ◽  
Large Magellanic Cloud ◽  
Star Formation History ◽  
Wide Field ◽  
Galactocentric Distance ◽  
Formation History ◽  
The Galaxy ◽  
History Of ◽  
Star Formation Histories

AbstractBased on the quantitative analysis of a set of wide-field color—magnitude diagrams reaching the old main sequence-turnoffs, we present new LMC star-formation histories, and their variation with galactocentric distance. Some coherent features are found, together with systematic variations of the star-formation history among the three fields analyzed. We find two main episodes of star formation in all three fields, from 1 to 4 and 7 to 13 Gyr ago, with relatively low star formation around ≃ 4–7 Gyr ago. The youngest age in each field gradually increases with galactocentric radius; in the innermost field, LMC 0514–6503, an additional star formation event younger than 1 Gyr is detected, with star formation declining, however, in the last ≃ 200 Myr. The population is found to be older on average toward the outer part of the galaxy, although star formation in all fields seems to have started around 13 Gyr ago.

scholarly journals Stellar Populations and the Star Formation Histories of LSB Galaxies—Part I: Optical and HαImaging

2011 ◽  
Vol 2011 ◽  
pp. 1-18 ◽  
Author(s):  
James Schombert ◽  
Tamela Maciel ◽  
Stacy McGaugh
Keyword(s):  
Star Formation ◽  
Data Storage ◽  
Star Formation History ◽  
Star Forming ◽  
Reduction Techniques ◽  
Formation History ◽  
History Of ◽  
Star Formation Histories ◽  
Baryonic Mass ◽  
Lsb Galaxies

This paper presents optical and Hαimaging for a large sample of LSB galaxies selected from the PSS-II catalogs (Schombert et al., 1992). As noted in previous work, LSB galaxies span a range of luminosities () and sizes (), although they are consistent in their irregular morphology. Their Hαluminosities (L(Hα)) range from 1036to 1041 ergs s−1(corresponding to a range in star formation, using canonical prescriptions, from 10−5to 1  yr−1). Although their optical colors are at the extreme blue edge for galaxies, they are similar to the colors of dwarf galaxies (Van Zee, 2001) and gas-rich irregulars (Hunter and Elmegreen, 2006). However, their star formation rates per unit stellar mass are a factor of ten less than other galaxies of the same baryonic mass, indicating that they are not simply quiescent versions of more active star-forming galaxies. This paper presents the data, reduction techniques, and new philosophy of data storage and presentation. Later papers in this series will explore the stellar population and star formation history of LSB galaxies using this dataset.

scholarly journals Sub-galactic scaling relations between X-ray luminosity, star formation rate, and stellar mass

2020 ◽  
Vol 494 (4) ◽  
pp. 5967-5984 ◽  
Author(s):  
K Kouroumpatzakis ◽  
A Zezas ◽  
P Sell ◽  
K Kovlakas ◽  
P Bonfini ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Star Formation History ◽  
High Mass ◽  
X Ray ◽  
Formation History ◽  
Low Mass ◽  
X Ray Binaries ◽  
Intrinsic Scatter

ABSTRACT X-ray luminosity (LX) originating from high-mass X-ray binaries (HMXBs) is tightly correlated with the host galaxy’s star formation rate (SFR). We explore this connection at sub-galactic scales spanning ∼7 dex in SFR and ∼8 dex in specific SFR (sSFR). There is good agreement with established relations down to SFR ≃ 10−3 M$_{\odot }\, \rm {yr^{-1}}$, below which an excess of X-ray luminosity emerges. This excess likely arises from low-mass X-ray binaries. The intrinsic scatter of the LX–SFR relation is constant, not correlated with SFR. Different star formation indicators scale with LX in different ways, and we attribute the differences to the effect of star formation history. The SFR derived from H α shows the tightest correlation with X-ray luminosity because H α emission probes stellar populations with ages similar to HMXB formation time-scales, but the H α-based SFR is reliable only for $\rm sSFR{\gt }10^{-12}$ M$_{\odot }\, \rm {yr^{-1}}$/M⊙.

scholarly journals Tracing the Mass‐Dependent Star Formation History of Late‐Type Galaxies Using X‐Ray Emission: Results from the Chandra Deep Fields

2008 ◽  
Vol 681 (2) ◽  
pp. 1163-1182 ◽  
Author(s):  
B. D. Lehmer ◽  
W. N. Brandt ◽  
D. M. Alexander ◽  
E. F. Bell ◽  
A. E. Hornschemeier ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Late Type ◽  
X Ray ◽  
Formation History ◽  
History Of ◽  
Deep Fields ◽  
Mass Dependent

scholarly journals The star formation history of the Magellanic Clouds

2008 ◽  
Vol 4 (S258) ◽  
pp. 51-60
Author(s):  
Carme Gallart ◽  
Ingrid Meschin ◽  
Noelia E. D. Noël ◽  
Antonio Aparicio ◽  
Sebastián L. Hidalgo ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Magellanic Clouds ◽  
Star Formation History ◽  
Galaxy Formation And Evolution ◽  
Formation History ◽  
History Of ◽  
General Studies ◽  
Star Formation Histories ◽  
The Impact

AbstractThe star formation history of the Magellanic Clouds, including the old and intermediate-age star formation events, can be studied reliably and in detail through color-magnitude diagrams reaching the oldest main sequence turnoffs. This paper reviews our current understanding of the Magellanic Clouds' star formation histories and discusses the impact of this information on general studies of galaxy formation and evolution.

The star-formation histories of early-type galaxies from ATLAS3D

2011 ◽  
Vol 7 (S284) ◽  
pp. 244-247 ◽  
Author(s):  
Richard M. McDermid ◽  
Katherine Alatalo ◽  
Leo Blitz ◽  
Maxime Bois ◽  
Frédéric Bournaud ◽  
...  
Keyword(s):  
Star Formation ◽  
Stellar Population ◽  
Abundance Ratio ◽  
Star Formation History ◽  
Early Type ◽  
Solar Abundance ◽  
Formation History ◽  
History Of ◽  
Free Parameters ◽  
Star Formation Histories

AbstractWe present an exploration of the integrated stellar populations of early-type galaxies (ETGs) from the ATLAS3D survey. We use two approaches: firstly the application of line-indices interpreted through single stellar population (SSP) models, which provide a single value of age, metallicity and abundance ratio. And secondly, by fitting a linear combination of SSP spectra to our data, smoothly weighted in the free parameters of age and metallicity, thereby inferring a star-formation history of these galaxies. Despite the significant differences in these approaches, we obtain generally consistent results, such that galaxies that are more massive appear older with enhanced abundance ratios using line indices, and have shorter star-formation histories weighted to early times. We highlight two limitations of the index-SSP approach. Firstly the SSP-equivalent ages belie the fact that ETGs are overwhelmingly composed of ancient stars. Secondly, the young stellar contributions implied in our star formation histories are required to obtain realistic UV-optical colours. We remark that, even fitting solar-abundance models, we can recover a star-formation duration that correlates with the measured alpha-enhancement, in agreement with other recent work.

scholarly journals X-ray Properties of Spiral Galaxies

2003 ◽  
Vol 214 ◽  
pp. 59-69
Author(s):  
Roberto Soria
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Supernova Remnants ◽  
Spiral Galaxies ◽  
Star Formation History ◽  
High Mass ◽  
X Ray ◽  
Formation History ◽  
Statistical Studies ◽  
X Ray Binaries

X-ray studies of nearby spiral galaxies with star formation allow us to investigate temperature and spatial distribution of the hot diffuse plasma, and to carry out individual and statistical studies of different classes of discrete sources (low- and high-mass X-ray binaries, Supernova remnants, supersoft and ultra-luminous sources). In particular, we briefly review the different models proposed to explain the ultra-luminous sources. We can then use the X-ray properties of a galaxy to probe its star formation history. We choose the starburst spiral M83 to illustrate some of these issues.

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