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PGC 14391
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Title: Improved method to determine the integrated properties of nuclear rings: NGC 1512
Author: Chao Ma, Richard de Grijs, Luis C. Ho

The integrated properties of nuclear rings are correlated with their host galaxy's secular evolution and its dynamics, as well as with the formation and evolution of the ring's star cluster population(s). Here we present a new method to accurately measure the spectral energy distribution and current star-formation rate (SFR) of the nuclear ring in the barred spiral galaxy NGC 1512 based on high-resolution Hubble and Spitzer Space Telescope images. Image degradation does not have a significant negative effect on the robustness of the results. To obtain the ring's SFR for the period spanning ~3--10 Myr, we apply our method to the continuum-subtracted H alpha and 8 m images. The resulting SFR surface density, Sigma_SFR=0.09 solar masses yr^-1 kpc^-2, which is much higher than the disk-averaged SFR densities in normal galaxies. We also estimate the ring's total stellar mass, log (M/solar masses) = 7.1 ± 0.11 for an average age of ~40 Myr.

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RE: NGC 1512
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Galaxy's snacking habits revealed

A team of Australian and Spanish astronomers have caught a greedy galaxy gobbling on its neighbours and leaving crumbs of evidence about its dietary past. Galaxies grow by churning loose gas from their surroundings into new stars, or by swallowing neighbouring galaxies whole. However, they normally leave very few traces of their cannibalistic habits.
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NGC 1512 (also ESO 250-4, IRAS 04022-4329, MCG -7-9-7 and PGC 14391) is a magnitude +11.1 face-on barred spiral galaxy located 41 million light-years away in the constellation Horologium.

The galaxy was discovered by Scottish astronomer James Dunlop using a  homemade 9-foot 22.86 cm (9 inch) f/12 speculum Newtonian reflector at Paramatta, New South Wales, Australia, on the 29th October 1826.

Position (J2000): R.A. 04h 03m 54.0s  |  Dec. -43° 20' 56"

It is a member of the Dorado Group.
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Title: XMM-Newton observation of the interacting galaxies NGC1512 and NGC1510
Author: L. Ducci (1, 2), P. J. Kavanagh (1), M. Sasaki (1), B. S. Koribalski (3) ((1) IAAT, University of Tübingen, (2) ISDC Genève, (3) ATNF, CSIRO Astronomy and Space Science)

The galaxy NGC1512 is interacting with the smaller galaxy NGC1510 and shows a peculiar morphology, characterised by two extended arms immersed in an HI disc whose size is about four times larger than the optical diameter of NGC1512. For the first time we performed a deep X-ray observation of the galaxies NGC1512 and NGC1510 with XMM-Newton to gain information on the population of X-ray sources and diffuse emission in a system of interacting galaxies. We identified and classified the sources detected in the XMM-Newton field of view by means of spectral analysis, hardness-ratios calculated with a Bayesian method, X-ray variability, and cross-correlations with catalogues in optical, infrared, and radio wavelengths. We also made use of archival Swift (X-ray) and Australia Telescope Compact Array (radio) data to better constrain the nature of the sources detected with XMM-Newton. We detected 106 sources in the energy range of 0.2-12 keV, out of which 15 are located within the D_25 regions of NGC1512 and NGC1510 and at least six sources coincide with the extended arms. We identified and classified six background objects and six foreground stars. We discussed the nature of a source within the D_25 ellipse of NGC1512, whose properties indicate a quasi-stellar object or an intermediate ultra-luminous X-ray source. Taking into account the contribution of low-mass X-ray binaries and active galactic nuclei, the number of high-mass X-ray binaries detected within the D_25 region of NGC1512 is consistent with the star formation rate obtained in previous works based on radio, infrared optical, and UV wavelengths. We detected diffuse X-ray emission from the interior region of NGC1512 with a plasma temperature of kT=0.68(0.31-0.87) keV and a 0.3-10 keV X-ray luminosity of 1.3E38 erg/s, after correcting for unresolved discrete sources.

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