Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...318..768v&link_type=abstract
Astronomy and Astrophysics, v.318, p.768-782
Astronomy and Astrophysics
Astrophysics
25
Galaxies: Ism, Galaxies: Individual: Ngc 4559, Galaxies: Spiral, X-Rays: Galaxies
Scientific paper
The inclined nearby (d=9.7Mpc) spiral galaxy NGC 4559 was observed with the ROSAT PSPC. Seventeen point sources were detected in a 15'x15' field, seven of which fall within the D_25_ ellipse of the galaxy. The most luminous source is associated with the nucleus of the galaxy, which has a luminosity of L_x_=7x10^39^erg/s and is slightly extended, suggesting a superposition of several compact sources or diffuse emission surrounding a compact central source. The source appears absorbed by a column of N_H_=10^21^cm^-2^ above the Galactic value, so that the intrinsic luminosity of the source exceeds the quoted value by about a factor two. No time variation of the X-ray emission from the central source or any other source in NGC 4559 could be established. The central X-ray source appears slightly offset from the optical center of the galaxy. The larger offset in the soft band may be due to partial shielding through the Hi disk of the emission from an extended distribution of X-ray binaries, or diffuse emission surrounding the center. Another bright source (L_x_=6x10^39^erg/s, N_H_=~1.7x10^21^cm^-2^, intrinsic L_x_>1.5x10^40^erg/s) was found in an outer spiral arm, coincident with an apparent group of HII regions. Since little radio or infrared emission emerges from this location, we conject that the X-rays originate from a single, several 100 year old buried supernova remnant that expands into gas with density of order 10^4^cm^-3^. Diffuse, unresolved emission within the galaxy's bulge and inner disk was detected with a total X-ray luminosity of L_x_=1.5x10^39^erg/s. Star formation activity at a rate of ~0.2Msun_/yr would produce sufficient X-ray emitting sources to account for this emission. However, the X-rays could also originate from globular cluster X-ray binaries without invoking recent star formation activity. No emission was detected from a possible halo. In the outer disk we detect a depression of soft X-rays that is likely caused by absorption of soft X-ray background radiation originating beyond the galaxy; the background surface brightness is estimated at S_x_>3x10^-4^cts/s/arcmin^2^. An upper limit of L_x_=1.9x10^38^erg/s was derived for the X-ray luminosity of the Type II SN 1941A.
Bertoldi Frank
Pietsch Wolfgang
Vögler Alexander
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