X-ray source variability study of the M 31 central field using<i>Chandra</i>HRC-I

Pietsch, W.; Henze, M.; Haberl, F.; Sturm, R.; Valle, M. Della; Hartmann, D. H.; Hatzidimitriou, D.

doi:10.1051/0004-6361/201321165

Cited by 21 publications

(54 citation statements)

References 80 publications

(142 reference statements)

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“…The better spatial resolution of Chandra allows to detect two different sources, about 8 ′′ apart, that contribute to the emission of the XMM-Newton XMM0042 source. Hofmann et al (2013) Note-We report the parameters of the best-fit constant+dips model of dipping XMM-Newton light curves of XMM0042 we analyzed. We show the observation number, number of dips, null hypothesis probability and the parameters as described in Section 2.…”

Section: Discussionmentioning

confidence: 99%

Discovery of Periodic Dips in the Brightest Hard X-Ray Source of M31 with EXTraS

Marelli¹,

Tiengo²,

Luca³

et al. 2017

ApJL

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We performed a search for eclipsing and dipping sources in the archive of the EXTraS project -a systematic characterization of the temporal behaviour of XMM-Newton point sources. We discovered dips in the X-ray light curve of 3XMM J004232.1+411314, which has been recently associated with the hard X-ray source dominating the emission of M31. A systematic analysis of XMM-Newton observations revealed 13 dips in 40 observations (total exposure time ∼0.8 Ms). Among them, four observations show two dips, separated by ∼4.01 hr. Dip depths and durations are variable. The dips occur only during low-luminosity states (L 0.2−12 < 1 × 10 38 erg s −1 ), while the source reaches L 0.2−12 ∼ 2.8 × 10 38 erg s −1 . We propose this system to be a new dipping Low-Mass X-ray Binary in M31 seen at high inclination (60• -80 • ), the observed dipping periodicity is the orbital period of the system. A blue HST source within the Chandra error circle is the most likely optical counterpart of the accretion disk. The high luminosity of the system makes it the most luminous dipper known to date.

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Section: Discussionmentioning

confidence: 99%

Discovery of Periodic Dips in the Brightest Hard X-Ray Source of M31 with EXTraS

Marelli¹,

Tiengo²,

Luca³

et al. 2017

ApJL

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“…13, we considered four catalogues: X-ray sources from Stiele et al (2011), deeper X-ray sources from Hofmann et al (2013), planetary nebulae from Ciardullo et al (1989), and UV sources from Rosenfield et al (2012). The UV sources studied by Rosenfield et al (2012) trace the old stellar population, and they have the same radial distribution as low-mass X-ray binaries, which correspond to the majority of the X-ray sources in Hofmann et al (2013). The stellar kinematics has been studied by Saglia et al (2010) with long slits: bulge stars exhibit a rotation with a maximum velocity of 100 km s −1 along the major axis (considered at PA = 48 deg) and a zero (systemic) velocity along the minor axis).…”

Section: Point Sources and Extinctionmentioning

confidence: 99%

“…The number of sources is significantly larger for Hofmann et al (2013) than for Stiele et al (2011); the former work is more sensitive as the data are stacked over a longer period. The work of Rosenfield et al (2012) Main physical parameters corresponding to the 13 CO(2-1) gas (left panel) and the C 18 O(2-1) gas (right panel) detected in M31-I(3).…”

Section: Point Sources and Extinctionmentioning

confidence: 99%

“…Thick ellipses show the approximate position of the inner ring. On the right side, we indicate, in the top panel, the number of X-ray sources (Hofmann et al 2013) detected at each radius; in the bottom panel, the X-ray luminosity at each radius is shown as a function of the radius. The mean and median values of the X-ray luminosity (averaged in 100 pc radial bin) is also provided.…”

Section: Point Sources and Extinctionmentioning

confidence: 99%

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Dense gas tracing the collisional past of Andromeda

Melchior

Combes

2015

A&A

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The central kiloparsec region of the Andromeda galaxy is relatively gas poor, while the interstellar medium appears to be concentrated in a ring-like structure at about 10 kpc radius. The central gas depletion has been attributed to a possible head-on collision 200 Myr ago, supported by the existence of an offset inner ring of warm dust. We present new IRAM 30 m radio telescope observations of the molecular gas in the central region, and the detection of CO and its isotopes 13 CO(2−1) and C 18 O(2−1), together with the dense gas tracers, HCN(1−0) and HCO+(1−0). A systematic study of the observed peak temperatures with non-local thermal equilibrium simulations shows that the detected lines trace dense regions with n H 2 in the range 2.5 × 10 4 −5.6 × 10 5 cm −3 , while the gas is very clumpy with a beam filling factor of 0.5−2 × 10 −2 . This is compatible with the dust mass derived from the far-infrared emission, assuming a dust-to-gas mass ratio of 0.01 with a typical clump size of 2 pc. We also show that the gas is optically thin in all lines except for 12 CO(1-0) and 12 CO(2-1), CO lines are close to their thermal equilibrium condition at 17-20 K, the molecular hydrogen density is larger than critical, and HCN and HCO+ lines have a subthermal excitation temperature of 9 K with a density smaller than critical. The average 12 CO/ 13 CO line ratio is high (∼21), and close to the 12 CO/C 18 O ratio (∼30) that was measured in the north-western region and estimated in the south-east stacking. The fact that the optically thin 13 CO and C 18 O lines have comparable intensities means that the secondary element 13 C is depleted with respect to the primary 12 C, as is expected just after a recent star formation. This suggests that there has been a recent starburst in the central region, supporting the head-on collision scenario.

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“…Regarding X-ray binaries, most sources have been classified based on correlations with lists of globular clusters, fewer through the detection of long-term variability (e. g. Trudolyubov et al 2006;Stiele et al 2008;Hofmann et al 2013), and only a few sources through the detection of short-term variability features, characteristic for X-ray binaries (Barnard et al 2003;.…”

Section: Introductionmentioning

confidence: 99%

NuSTAR view of the central region of M31

Stiele

Kong

2018

Monthly Notices of the Royal Astronomical Society

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Our neighbouring large spiral galaxy, the Andromeda galaxy (M 31 or NGC 224), is an ideal target to study the X-ray source population of a nearby galaxy. NuSTAR observed the central region of M 31 in 2015 and allows studying the population of X-ray point sources at energies higher than 10 keV. Based on the source catalogue of the large XMM-Newton survey of M 31, we identified counterparts to the XMM-Newton sources in the NuSTAR data. The NuSTAR data only contain sources of a brightness comparable (or even brighter) than the selected sources that have been detected in XMM-Newton data. We investigate hardness ratios, spectra and long-term light curves of individual sources obtained from NuSTAR data. Based on our spectral studies we suggest four sources as possible X-ray binary candidates. The long-term light curves of seven sources that have been observed more than once show low (but significant) variability.

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X-ray source variability study of the M 31 central field usingChandraHRC-I

Cited by 21 publications

References 80 publications

Discovery of Periodic Dips in the Brightest Hard X-Ray Source of M31 with EXTraS

Discovery of Periodic Dips in the Brightest Hard X-Ray Source of M31 with EXTraS

Dense gas tracing the collisional past of Andromeda

NuSTAR view of the central region of M31

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