Radio observations of NGC 6388: an upper limit on the mass of its central black hole

Cseh, D.; Kaaret, P.; Corbel, S.; Körding, Elmar; Coriat, M.; Tzioumis, A. K.; Lanzoni, B.

doi:10.1111/j.1365-2966.2010.16726.x

Cited by 35 publications

(44 citation statements)

References 53 publications

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“…and averaged quiescent luminosities of L X 10 32 −10 33 erg/s. The relatively small uncertainty in the position of IGR J17361-4441, as determined thanks to the Chandra observation of the source carried out by Pooley et al (2011), suggests that the newly discovered INTEGRAL transient is associated with neither the objects detected previously in quiescence by Cseh et al (2010), nor the COG of NGC 6388 (see Fig. 5).…”

Section: Discussionmentioning

confidence: 99%

“…To date, the deepest X-ray observations of the GC were carried out with Chandra and reported by Cseh et al (2010). These authors found a number of sources located close to the core of the GC (sources #3, #7, and #12), with spectral properties similar to those of the X-ray binaries 4 .…”

Section: Discussionmentioning

confidence: 99%

“…(2) of Cseh et al (2010) and taking into account the intrinsic scatter in the fundamental plane relation, the newly derived upper limit to the IMBH mass is M < 600 M . This is a factor of 2.5 smaller than that reported by Cseh et al (2010).…”

Section: Discussionmentioning

confidence: 99%

“…2.4 gives a significantly tighter constraint of the allowed mass for this object with respect to those reported previously. Following the discussion in Cseh et al (2010), we assume that the quiescent X-ray luminosity of the IMBH is that determined by these authors with Chandra and consider the updated L R provided by our ATCA ToO observation. Inserting these values into Eq.…”

Section: Discussionmentioning

confidence: 99%

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IGR J17361-4441: a possible new accreting X-ray binary in NGC 6388

Bozzo

Ferrigno

Stevens

et al. 2011

A&A

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IGR J17361-4441 is a newly discovered INTEGRAL hard X-ray transient, located in the globular cluster NGC 6388. We report here the results of the X-ray and radio observations performed with Swift, INTEGRAL, RXTE, and the Australia Telescope Compact Array (ATCA) after the discovery of the source on 2011 August 11. In the X-ray domain, IGR J17361-4441 showed virtually constant flux and spectral parameters up to 18 days from the onset of the outburst. The broad-band (0.5-100 keV) spectrum of the source could be reasonably well described by using an absorbed power-law component with a high energy cut-off (N H 0.8 × 10 22 cm −2 , Γ 0.7-1.0, and E cut 25 keV) and displayed some evidence of a soft component below ∼2 keV. No coherent timing features were found in the RXTE data. The ATCA observation did not detect significant radio emission from IGR J17361-4441, and provided the most stringent upper limit (rms 14.1 μJy at 5.5 GHz) to date on the presence of any radio source close to the NGC 6388 center of gravity. The improved position of IGR J17361-4441 in outburst determined from a recent target of opportunity observation with Chandra, together with the X-ray flux and radio upper limits measured in the direction of the source, argue against its association with the putative intermediate-mass black hole residing in the globular cluster and with the general hypothesis that the INTEGRAL source is a black hole candidate. IGR J17361-4441 might be more likely a new X-ray binary hosting an accreting neutron star. The ATCA radio non-detection also permits us to derive an upper limit to the mass of the suspected intermediate massive black hole in NGC 6388 of 600 M . This is a factor of 2.5 lower than the limit reported previously.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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IGR J17361-4441: a possible new accreting X-ray binary in NGC 6388

Bozzo

Ferrigno

Stevens

et al. 2011

A&A

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“…This issue was considered by several authors. For example, Grindlay et al (2001) provided the census of the compact objects and binary populations in the globular cluster 47 Tuc and obtained an upper limit to the central IMBH of a few hundred solar masses; Nucita et al (2008) showed that the core of the globular cluster NGC 6388 harbors several X-ray sources; and Cseh et al (2010) refined the analysis putting an upper limit to the central IMBH mass of a few thousand solar masses (see also Bozzo et al 2011;Nucita et al 2012).…”

Section: An Intermediate-mass Black Hole In the Fornax Galaxy: High-ementioning

confidence: 99%

AnXMM-Newtonsearch for X-ray sources in the Fornax dwarf galaxy

Nucita

Manni

Paolis

et al. 2013

A&A

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We report the results of a deep archive XMM-Newton observation of the Fornax spheroidal galaxy that we analyzed with the aim of fully characterizing the X-ray source population (in most of the cases likely to be background active galactic nuclei) detected towards the target. A cross correlation with the available databases allowed us to find a source that may be associated with a variable star belonging to the galaxy. We also searched for X-ray sources in the vicinity of the Fornax globular clusters GC 3 and GC 4 and found two sources probably associated with the respective clusters. The deep X-ray observation was also suitable for the search of the intermediate-mass black hole (of mass 10 4 M ) expected to be hosted in the center of the galaxy. In the case of Fornax, this search is extremely difficult since the galaxy centroid of gravity is poorly constrained because of the large asymmetry observed in the optical surface brightness. Since we cannot firmly establish the existence of an X-ray counterpart of the putative black hole, we put constraints only on the accretion parameters. In particular, we found that the corresponding upper limit on the accretion efficiency, with respect to the Eddington luminosity, is as low as a few 10 −5 .

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Searching for IMBHs in Galactic globular clusters through radial velocities of individual stars

Lanzoni

2014

Proc. IAU

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Abstract. I present an overview of our ongoing project aimed at building a new generation of velocity dispersion profiles ad rotation curves for a representative sample of Galactic globular clusters, from the the radial velocity of hundreds of individual stars distributed at different distances from the cluster center. The innermost portion of the profiles will be used to constrain the possible presence of intermediate-mass black holes. The adopted methodology consists of combining spectroscopic observations acquired with three different instruments at the ESO-VLT: the adaptive-optics assisted, integral field unit (IFU) spectrograph SINFONI for the innermost and highly crowded cluster cores, the multi-IFU spectrograph KMOS for the intermediate regions, and the multi-fiber instrument FLAMES/GIRAFFE-MEDUSA for the outskirts. The case of NGC 6388, representing the pilot project that motivated the entire program, is described in some details.

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Radio observations of NGC 6388: an upper limit on the mass of its central black hole

Cited by 35 publications

References 53 publications

IGR J17361-4441: a possible new accreting X-ray binary in NGC 6388

IGR J17361-4441: a possible new accreting X-ray binary in NGC 6388

AnXMM-Newtonsearch for X-ray sources in the Fornax dwarf galaxy

Searching for IMBHs in Galactic globular clusters through radial velocities of individual stars

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