Low-mass X-ray binaries as a stellar mass indicator for the host galaxy

By M. Gilfanov. 2004

258 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/c87728e0dcfde234996906f18a61f81a9a380173

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In Astronomy and Astrophysics

Citations in the corpus

THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE (2009, unknown): “…power laws with α ∼ 2.5 have been observed in flat spectrum radio quasars, and at low luminosities very shallow power laws with α ∼ 1.2 have been measured in LMXB populations (Grimm et al. 2003; Gilfanov 2004; Kim & Fabbiano 2004; Voss & Gilfanov 2006; Padovani et al. 2007; Abdo et al. 2009a).”
X-ray emission from star-forming galaxies – I. High-mass X-ray binaries (2011, methodology): “For M101 the bulge region was chosen based on results from Gilfanov (2004).”
X-ray emission from star-forming galaxies - II. Hot interstellar medium (2012, methodology): “In early-type galaxies, the number and luminosity of low-mass X-ray binaries (LMXBs) scale well with the stellar mass of the galaxy (Gilfanov 2004).”
The distances to Galactic low-mass X-ray binaries: consequences for black hole luminosities and kicks (2004, background): “Furthermore, Gilfanov (2004) found that the distribution of LMXBs follows the stellar mass distribution, and hence not the spiral arm structure.”
The Type Ia Supernova Rate (2005, background): “This is an important clue that SNe Ia have two evolutionary channels with different characteristic times: one " prompt, " basically tracking the current SFR, and another so delayed that it appears to simply track the stellar mass [much as is seen in accreting binaries with low-mass companions, such ”
A COMPLETE SAMPLE OF ULTRALUMINOUS X-RAY SOURCE HOST GALAXIES (2011, methodology): “The ULX number density per unit mass and SFR of their host galaxies are consistent with the extrapolation of the luminosity function of ordinary X-ray binaries (Grimm et al. 2003; Gilfanov 2004).”
A global spectral study of black hole X-ray binaries (2009, methodology): “The level of this X-ray binary emission has been used as a proxy for the star formation rate of the galaxy (e.g. Grimm et al. 2003) as well as the stellar mass (e.g. Gilfanov 2004).”
Compact Object Modeling with the StarTrack Population Synthesis Code (2005, background): “…may also result in an independent diagnostic of star formation rates for nearby galaxies, since both the numbers and properties of XRBs are directly connected to the star formation history (see, e.g., Grimm et al. 2003; Gilfanov 2004; Kim & Fabbiano 2004; K. Belczynski et al. 2008, in preparation).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, background): “We also assume that the LMXB emission follows the Ks band light (see also Gilfanov 2004).”
A CHANDRA PERSPECTIVE ON GALAXY-WIDE X-RAY BINARY EMISSION AND ITS CORRELATION WITH STAR FORMATION RATE AND STELLAR MASS: NEW RESULTS FROM LUMINOUS INFRARED GALAXIES (2010, methodology): “Using simple polynomial fitting techniques, 10 However, see Grimm et al. (2003), Gilfanov et al. (2004a), and Gilfanov (2004) for different scalings depending onM⋆ and SFR regimes. we find for galaxies with SFR<∼ 5 M⊙ yr −1, M⋆ and SFR are nearly linearly correlated (M⋆ ∝ SFR 1.10); however, for gal”
High-mass X-ray binaries in the Milky Way (2013, methodology): “Therefore indirect methods, such as the construction of X-ray luminosity functions (LF), are needed to study of properties of populations of sources located in different regions of a galaxy (see, e.g., Gilfanov, 2004; Mineo et al., 2012a).”
Populations of X-Ray Sources in Galaxies (2006, background): “In the case of Chandra the detection efficiency is also affected by the radial dependence of the degradation of the mirror resolution off-axis (see Kim & Fabbiano 2003, 2004; Gilfanov 2004).”
X-ray luminosity function of faint point sources in the Milky Way (2005, methodology): “Gilfanov (2004) subsequently demonstrates that the LMXB XLFs for 11 nearby galaxies and the Milky Way have a universal shape and normalizations that are proportional to the stellar masses.”
REVISITING WITH CHANDRA THE SCALING RELATIONS OF THE X-RAY EMISSION COMPONENTS (BINARIES, NUCLEI, AND HOT GAS) OF EARLY-TYPE GALAXIES (2010, methodology): “…LX range may be characterized by multiple PLs (see Figure 3 in Kim & Fabbiano 2010), one of the key features is that the XLF shape is more or less fixed with a universal slope of ∼1 (in the form of dN/dln LX) between LX = 5 × 1037 erg s−1 and 5 × 1038 erg s−1 (Kim & Fabbiano 2004; Gilfanov 2004).”
X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, background): “…2005; Lehmer et al. 2010; Mineo et al. 2012a), as well as a scaling between total X-ray emission from low-mass XRBs (LMXBs) and stellar mass (M∗) (Gilfanov 2004; Lehmer et al. 2010; Boroson et al. 2011; Zhang et al. 2012). tfragos@cfa.harvard.edu 1 Harvard-Smithsonian Center for Astrophysics,…”
Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, methodology): “The normalization f the HMXB LF is proportional to the SFR; the normalization of the LMXB LF is proportional to the stellar mass (Gilfanov et al. 2004; Gilfanov 2004).”