The Milky Way in X-rays for an outside observer

By H. Grimm, M. Gilfanov, R. Sunyaev, Max-Planck-Institut fuer Astrophysik, Space Reseach Institute. 2001

308 citations recorded by the source corpus.

A method of simultaneous production of phthalic anhydride and anthraquinone, consisting in a vapour-phase oxidation of a stock material which is a mixture of naphthalene and anthracene by atmospheric oxygen in a stationary bed of a vanadium catalyst. The oxidation is carried out at a space rate of feed of said mixture equal to 50-120 g/hour per litre of the catalyst and at a stock-to-air ratio of 0.03-0.08 g/litre.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bcb93170605bef465e8c2b6d50e9a0f6c49cf101

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1. C. Steidel
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Citations in the corpus

• INTEGRAL/IBIS all-sky survey in hard X-rays (2007, background): “11), is much flatter than that of extragalactic sources at |b| > 5◦ (Forman et al. 1978) and reflects the luminosity functions of the dominant Galactic source populations (see e.g. Grimm et al. 2002).”
• The Spiral Arms and Interarm Separation of the Milky Way: An Updated Statistical Study (2005, background): “Grimm et al. (2002) found a clear signature of the spiral arms in the spatial distribution of high-mass X-ray-emitting binary stars.”
• X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, background): “This is not an unexpected result, given that in the Milky Way, which is a typical spiral galaxy, there are only a few HMXBs with luminosity above 1037ergs−1 (Grimm et al. 2002; Voss & Ajello 2010).”
• TOWARD A UNIFICATION OF STAR FORMATION RATE DETERMINATIONS IN THE MILKY WAY AND OTHER GALAXIES (2011, methodology): “We also add the luminosity of the Crab Nebula (LX = 1 × 10 38 erg s−1 assuming a distance of 2 kpc; Grimm et al. 2002; Davidson & Fesen 1985), which dominates the Milky Way’s SNR luminosity in the X-ray band.”
• The 511 keV emission from positron annihilation in the Galaxy (2010, background): “…by SPI/INTEGRAL, Prantzos (2004) noticed that i) the observed distribution of LMXRBs in the Galaxy is strongly peaked towards the central regions (Grimm et al., 2002), similar to that of the 511 keV emission, and ii) their total X-ray luminosity is ∼1039 erg s−1, a hundred times larger than the…”
• Low-mass X-ray binaries as a stellar mass indicator for the host galaxy (2004, methodology): “These expectations are supported by the spatial distribution of the compact X-ray sources in the disks of spiral galaxies, which often show a concentration towards the spiral arms (e.g. Pence et al. 2001; Grimm et al. 2002).”
• The all-sky distribution of 511 keV electron-positron annihilation emission (2005, background): “The two classes show clearly different spatial distributions (Grimm et al. 2002).”
• High-mass X-ray binaries in the Milky Way (2013, methodology): “1; see also e.g. Grimm et al., 2002).”
• Formation of Double Neutron Star Systems (2017, methodology): “We argued that few, if any, of the presently known Galactic HMXBs will survive their subsequent CE evolution and eventually produce a DNS system.”
• A Census of Optical and Near-Infrared Selected Star-forming and Passively Evolving Galaxies at Redshift z ~ 2 (2005, background): “The X-ray luminosity of local non-active galaxies results primarily from high mass X-ray binaries, supernovae, and diffuse hot gas (e.g., Grimm et al. 2002; Strickland et al. 2004); all of these sources of X-ray emission are related to the star formation activity on timescales of .”
• X-Ray Luminosity Function and Total Luminosity of Low-Mass X-Ray Binaries in Early-Type Galaxies (2003, methodology): “For example, for a given LB of the Milky Way bulge, we expect only a few LMXBs with LX > 1038 erg s-1, consistent with observations (e.g., Grimm et al. 2002) In both the M31 and the Milky Way LMXB XLFs, there is a low luminosity break near LX ~ 1037 erg s-1, and the slope flattens considerably at…”
• Gamma-ray binaries and related systems (2013, methodology): “The X-ray sources are not exceptionally bright: there are ∼> 100 Xray sources in the Galactic Plane, typically accreting X-ray binaries, that are brighter than LS I +61◦303 (compare the mean count rate of 0.2 counts s−1 reported in Paredes et al. 1997 to the logN-log S derived from the RXTE/ASM by G”
• The distances to Galactic low-mass X-ray binaries: consequences for black hole luminosities and kicks (2004, background): “It is clear that few LMXBs at the other side of the Galactic Centre have been detected, especially if the Eddington limit for hydrogen rich material for a 1.4 M⊙ neutron star is applicable to the peak burst flux of most photospheric radius expansion bursts (see also Grimm et al. 2002).”
• Old and Young X-Ray Point Source Populations in Nearby Galaxies (2003, methodology): “Based on the XRB populations in our Galaxy, one might therefore suppose that the correlations merely represent an extrapolation of the total X-ray luminosity from the LMXB and HMXB populations, scaled to the galaxy mass and SFR (e.g., Grimm et al. 2002).”