IGR J16194–2810: a new symbiotic X-ray binary

Masetti, N.; Landi, R.; Pretorius, Magaretha L.; Sguera, V.; Bird, A. J.; Perri, M.; Charles, P. A.; Kennea, J. A.; Malizia, A.; Ubertini, P.

doi:10.1051/0004-6361:20077509

Cited by 97 publications

(112 citation statements)

References 51 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This confirms the importance of this identification work on catalogued but unidentified high-energy sources, because peculiar objects can be found within the considered samples (see, for instance, Paper IX; Masetti et al 2007Masetti et al , 2008bBassani et al 2012;de Martino et al 2010de Martino et al , 2013. With the present data, we also correct two results given in Paper IX, namely the actual redshift (z = 2.02) of the Type 1 QSO IGR J16388+3557 and the correct counterpart of source IGR J06293−1359.…”

Section: Discussionsupporting

confidence: 88%

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

Self Cite

View full text Add to dashboard Cite

Within the framework of our program (running since 2004) of identification of hard X-ray INTEGRAL sources through optical spectroscopy, we present the results concerning the nature of 33 high-energy objects. The data were acquired with the use of six telescopes of different sizes and from one on-line archive. The results indicate that the majority of these objects (23 out of 33) are active galactic nuclei (AGNs), whereas 10 are sources in the local Universe with eight of which in the Galaxy and two in the Small Magellanic Cloud (SMC). Among the identified AGNs, 13 are of Type 1 (i.e., with broad emission lines), eight are of Type 2 (with narrow emissions only), and two are X-ray bright, optically normal galaxies with no apparent nuclear activity in the optical. Six of these AGNs lie at high redshift (z > 0.5). Concerning local objects, we found that five of them are Galactic cataclysmic variables, three are high-mass X-ray binaries (two of which lying in the SMC), one is a low-mass X-ray binary, and one is classified as a flare star that is likely of RS CVn type. The main optical properties and inferred physical characteristics of these sources are presented and discussed.

show abstract

Section: Discussionsupporting

confidence: 88%

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Currently, only 8 of such symbiotic X-ray binaries have been identified (e.g., Masetti et al 2007;Nespoli et al 2010). All of these systems show both long-and short-term X-ray variability and are characterized by 2-10 keV luminosities ranging between ∼10 32−35 erg s −1 , although one object shows more intense X-ray emission of L X ∼ 10 36−37 erg s −1 (e.g., Masetti et al 2007). However, for the extinction towards XMM J174457-2850.3 and a distance of 8 kpc, an M-type giant would have a magnitude of K s ∼ 11−13 mag (Drilling & Landolt 2000;Tokunaga 2000).…”

Section: Xmm J174457-28503: a Wind-fed System?mentioning

confidence: 99%

A four-year baselineSwiftstudy of enigmatic X-ray transients located near the Galactic center

Degenaar

Wijnands

2010

A&A

108

View full text Add to dashboard Cite

We report on continued monitoring observations of the Galactic center carried out by the X-ray telescope aboard the Swift satellite in 2008 and 2009. This campaign revealed activity of the five known X-ray transients AX J1745.6-2901, CXOGC J174535.5-290124, GRS 1741-2853, XMM J174457-2850.3 and CXOGC J174538.0-290022. All these sources are known to undergo very faint X-ray outbursts with 2-10 keV peak luminosities of L X,peak ∼ 10 34−36 erg s −1 , although the two confirmed neutron star low-mass X-ray binaries AX J1745.6-2901 and GRS 1741-2853 can also become brighter (L X,peak ∼ 10 36−37 erg s −1 ). We discuss the observed longterm lightcurves and X-ray spectra of these five enigmatic transients. In 2008, AX J1745.6-2901 returned to quiescence following an unusually long accretion outburst of more than 1.5 years. GRS 1741-2853 was active in 2009 and displayed the brightest outburst ever recorded for this source, reaching up to a 2-10 keV luminosity of L X ∼ 1 × 10 37 (D/7.2 kpc) 2 erg s −1 . This system appears to undergo recurrent accretion outbursts approximately every 2 years. Furthermore, we find that the unclassified transient XMM J174457-2850.3 becomes bright only during short episodes (days) and is often found active in between quiescence (L X ∼ 10 32 erg s −1 ) and its maximum outburst luminosity of L X ∼ 10 36 erg s −1 . CXOGC J174535.5-290124 and CXOGC J174538.0-290022, as well as three other veryfaint X-ray transients that were detected by Swift monitoring observations in 2006, have very low time-averaged mass-accretion rates of Ṁ long < ∼ 2 × 10 −12 M yr −1 . Despite having obtained two years of new data in 2008 and 2009, no new X-ray transients were detected.

show abstract

“…While we know of several symbiotic X-ray binaries with neutron star accretors (see, e.g., Masetti et al 2007;Corbet et al 2008;Enoto et al 2014), and symbiotic stars with main sequence accretors may exist, the majority of symbiotic stars appear to be wide binaries in which white dwarfs accrete from red giants.…”

Section: Introductionmentioning

confidence: 99%

SU Lyncis, a hard X-ray bright M giant: clues point to a large hidden population of symbiotic stars

Mukai

Luna

Cusumano

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

110

View full text Add to dashboard Cite

Symbiotic star surveys have traditionally relied almost exclusively on low resolution optical spectroscopy. However, we can obtain a more reliable estimate of their total Galactic population by using all available signatures of the symbiotic phenomenon. Here we report the discovery of a hard X-ray source, 4PBC J0642.9+5528, in the Swift hard X-ray all-sky survey, and identify it with a poorly studied red giant, SU Lyn, using pointed Swift observations and ground-based optical spectroscopy. The X-ray spectrum, the optical to UV spectrum, and the rapid UV variability of SU Lyn are all consistent with our interpretation that it is a symbiotic star containing an accreting white dwarf. The symbiotic nature of SU Lyn went unnoticed until now, because it does not exhibit emission lines strong enough to be obvious in low resolution spectra. We argue that symbiotic stars without shell-burning have weak emission lines, and that the current lists of symbiotic stars are biased in favor of shell-burning systems. We conclude that the true population of symbiotic stars has been underestimated, potentially by a large factor.

show abstract

IGR J16194–2810: a new symbiotic X-ray binary

Cited by 97 publications

References 51 publications

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Unveiling the nature of INTEGRAL objects through optical spectroscopy

A four-year baselineSwiftstudy of enigmatic X-ray transients located near the Galactic center

SU Lyncis, a hard X-ray bright M giant: clues point to a large hidden population of symbiotic stars

Contact Info

Product

Resources

About