Exploring the X-ray universe via timing: mass of the active galactic nucleus black hole XMMUJ134736.6+173403

2019 ◽  
Vol 15 (S356) ◽  
pp. 348-350
Author(s):  
Eva Šrámková ◽  
K. Goluchová ◽  
G. Török ◽  
Marek A. Abramowicz ◽  
Z. Stuchlík ◽  
...  
Keyword(s):  
Black Hole ◽  
Frequency Ratio ◽  
Active Galactic Nucleus ◽  
Periodic Modulation ◽  
X Ray ◽  
Upper Limit ◽  
M 10 ◽  
Frequency Ratios ◽  
Quasiperiodic Oscillations ◽  
Twin Peak

AbstractA strong quasi-periodic modulation has recently been revealed in the X-ray flux of the X-ray source XMMUJ134736.6+173403. The two observed twin-peak quasiperiodic oscillations (QPOs) exhibit a 3:1 frequency ratio and strongly support the evidence for the presence of an active galactic nucleus black hole (AGN BH). It has been suggested that detections of twin-peak QPOs with commensurable frequency ratios and scaling of their periods with BH mass could provide the basis for a method intended to determine the mass of BH sources, such as AGNs. Assuming the orbital origin of QPOs, we calculate the upper and lower limit on the AGN BH mass M, reaching M ≍ 107–109M⊙. Compared to mass estimates of other sources, XMMUJ134736.6+173403 appears to be the most massive source with commensurable QPO frequencies, and its mass represents the current observational upper limit on the AGN BH mass obtained from the QPO observations.

scholarly journals Mass of the active galactic nucleus black hole XMMUJ134736.6+173403

2019 ◽  
Vol 622 ◽  
pp. L8 ◽  
Author(s):  
K. Goluchová ◽  
G. Török ◽  
E. Šrámková ◽  
M. A. Abramowicz ◽  
Z. Stuchlík ◽  
...  
Keyword(s):  
Black Hole ◽  
Lower Limit ◽  
Frequency Ratio ◽  
Active Galactic Nucleus ◽  
Periodic Modulation ◽  
Resonance Model ◽  
X Ray ◽  
Harmonic Sequence ◽  
Upper Limit ◽  
Quasiperiodic Oscillations

A recent study of the X-ray source XMMUJ134736.6+173403 has revealed a strong quasi-periodic modulation in the X-ray flux. The observation of two quasiperiodic oscillations (QPOs) that occur on a daily timescale and exhibit a 3:1 frequency ratio strongly supports the evidence for the presence of an active galactic nucleus black hole (AGN BH). Assuming an orbital origin of QPOs, we calculated the upper and lower limit on AGN BH mass M and found M ≈ 107 − 109 M⊙. When we compare this to mass estimates of other sources, XMMUJ134736.6+173403 appears to be the most massive source with commensurable QPO frequencies, and its mass represents the current observational upper limit on AGN BH mass based on QPO observations. We note that it will be crucial for the falsification of particular resonance models of QPOs whether only a single QPO with a frequency that completes the harmonic sequence 3 : 2 : 1 is found in this source, or if a new different pair of QPOs with frequencies in the 3 : 2 ratio is found. The former case would agree with the prediction of the 3 : 2 epicyclic resonance model and BH mass M ≈ (5a2 + 8a + 8)×107 M⊙, where a is a dimensionless BH spin.

scholarly journals X-Ray Determination of the Black-Hole Mass in Cygnus X-1

1998 ◽  
Vol 188 ◽  
pp. 388-389
Author(s):  
A. Kubota ◽  
K. Makishima ◽  
T. Dotani ◽  
H. Inoue ◽  
K. Mitsuda ◽  
...  
Keyword(s):  
Black Hole ◽  
Compact Object ◽  
Optical Observations ◽  
Black Hole Mass ◽  
X Ray ◽  
Upper Limit ◽  
Supergiant Star ◽  
X Ray Binaries ◽  
Two Bodies

About 10 X-ray binaries in our Galaxy and LMC/SMC are considered to contain black hole candidates (BHCs). Among these objects, Cyg X-1 was identified as the first BHC, and it has led BHCs for more than 25 years(Oda 1977, Liang and Nolan 1984). It is a binary system composed of normal blue supergiant star and the X-ray emitting compact object. The orbital kinematics derived from optical observations indicates that the compact object is heavier than ~ 4.8 M⊙ (Herrero 1995), which well exceeds the upper limit mass for a neutron star(Kalogora 1996), where we assume the system consists of only two bodies. This has been the basis for BHC of Cyg X-1.

scholarly journals Estimation of the jet inclination angle for the TDE Swift J1644+57

2019 ◽  
Vol 492 (2) ◽  
pp. 1634-1640
Author(s):  
Sudip Chakraborty ◽  
Sudip Bhattacharyya ◽  
Chandrachur Chakraborty ◽  
A R Rao
Keyword(s):  
Black Hole ◽  
Data Analysis ◽  
Inclination Angle ◽  
Jet Physics ◽  
Triggering Mechanism ◽  
Tidal Disruption ◽  
X Ray ◽  
Upper Limit ◽  
The One ◽  
Disruption Event

ABSTRACT An estimate of the jet inclination angle relative to the accreting black hole’s spin can be useful to probe the jet triggering mechanism and the disc–jet coupling. A tidal disruption event (TDE) of a star by a supermassive spinning black hole provides an excellent astrophysical laboratory to study the jet direction through the possibility of jet precession. In this work, we report a new method to constrain the jet inclination angle β and apply it to the well-sampled jetted TDE Swift J1644+57. This method involves X-ray data analysis and comparisons of jet models with broad properties of the observed X-ray dips, to estimate the upper limit of the extent of the contribution of a plausible jet precession to these X-ray dips. From this limit, we find that β is very likely to be less than ∼15° for Swift J1644+57. Such a well-constrained jet inclination angle could be useful to probe the jet physics. The main advantage of our method is that it does not need to assume an origin of the observed X-ray dips, and the conclusion does not depend on any particular type of jet precession (e.g. the one due to the Lense–Thirring effect) or any specific value of precession frequency or any particular jet model. These make this method reliable and applicable to other jetted TDEs, as well as to other jetted accreting systems.

scholarly journals The stringent upper limit on jet power in the persistent soft-state source 4U 1957+11

2020 ◽  
Vol 498 (1) ◽  
pp. L40-L45
Author(s):  
Thomas J Maccarone ◽  
Arlo Osler ◽  
James C A Miller-Jones ◽  
P Atri ◽  
David M Russell ◽  
...  
Keyword(s):  
Black Hole ◽  
Type I ◽  
X Ray ◽  
Upper Limit ◽  
Source Distance ◽  
Upper Limits ◽  
Soft State ◽  
Hard State ◽  
Comprehensive Search ◽  
Radio Power

ABSTRACT We present extremely deep upper limits on the radio emission from 4U 1957+11, an X-ray binary that is generally believed to be a persistently accreting black hole that is almost always in the soft state. We discuss a more comprehensive search for Type I bursts than in past work, revealing a stringent upper limit on the burst rate, bolstering the case for a black hole accretor. The lack of detection of this source at the 1.07 μJy/beam noise level indicates jet suppression that is stronger than expected even in the most extreme thin disc models for radio jet production – the radio power here is 1500–3700 times lower than the extrapolation of the hard state radio/X-ray correlation, with the uncertainties depending primarily on the poorly constrained source distance. We also discuss the location and velocity of the source and show that it must have either formed in the halo or with a strong asymmetric natal kick.

A remark about possible unity of the neutron star and black hole high frequency QPOs

Open Physics ◽  
2007 ◽  
Vol 5 (4) ◽  
Author(s):  
Gabriel Török ◽  
Zdeněk Stuchlík ◽  
Pavel Bakala
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
High Frequency ◽  
Physical Mechanism ◽  
General Trend ◽  
X Ray ◽  
Quasiperiodic Oscillations

AbstractIn a series of papers it was discussed,on the basis of phenomenological arguments, whether the high frequency quasiperiodic oscillations (kHz QPOs)observed in the neutron-star and black-hole X-ray sources originate in the same physical mechanism. Recently it was suggested that a general trend seen in neutron star kHz QPOs instead excludes such a uniform origin. Using the example of the atoll source 4U 1636-53 we illustrate that this is not neccesarily true.

scholarly journals Models of high-frequency quasi-periodic oscillations and black hole spin estimates in Galactic microquasars

2020 ◽  
Vol 643 ◽  
pp. A31
Author(s):  
A. Kotrlová ◽  
E. Šrámková ◽  
G. Török ◽  
K. Goluchová ◽  
J. Horák ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
High Frequency ◽  
Accretion Disc ◽  
The Other ◽  
Periodic Oscillations ◽  
X Ray ◽  
Upper Limit ◽  
Oscillation Modes

We explore the influence of nongeodesic pressure forces present in an accretion disc on the frequencies of its axisymmetric and nonaxisymmetric epicyclic oscillation modes. We discuss its implications for models of high-frequency quasi-periodic oscillations (QPOs), which have been observed in the X-ray flux of accreting black holes (BHs) in the three Galactic microquasars, GRS 1915+105, GRO J1655−40, and XTE J1550−564. We focus on previously considered QPO models that deal with low-azimuthal-number epicyclic modes, |m| ≤ 2, and outline the consequences for the estimations of BH spin, a ∈ [0, 1]. For four out of six examined models, we find only small, rather insignificant changes compared to the geodesic case. For the other two models, on the other hand, there is a significant increase of the estimated upper limit on the spin. Regarding the falsifiability of the QPO models, we find that one particular model from the examined set is incompatible with the data. If the spectral spin estimates for the microquasars that point to a >  0.65 were fully confirmed, two more QPO models would be ruled out. Moreover, if two very different values of the spin, such as a ≈ 0.65 in GRO J1655−40 and a ≈ 1 in GRS 1915+105, were confirmed, all the models except one would remain unsupported by our results. Finally, we discuss the implications for a model that was recently proposed in the context of neutron star (NS) QPOs as a disc-oscillation-based modification of the relativistic precession model. This model provides overall better fits of the NS data and predicts more realistic values of the NS mass compared to the relativistic precession model. We conclude that it also implies a significantly higher upper limit on the microquasar’s BH spin (a ∼ 0.75 vs. a ∼ 0.55).

scholarly journals Discovery of a transient X-ray source Suzaku J1305−4930 in NGC 4945

2020 ◽  
Vol 72 (3) ◽  
Author(s):  
Shuntaro Ide ◽  
Kiyoshi Hayashida ◽  
Hirofumi Noda ◽  
Hiroyuki Kurubi ◽  
Tomokage Yoneyama ◽  
...  
Keyword(s):  
Black Hole ◽  
Absorption Feature ◽  
Power Law Model ◽  
Disk Model ◽  
Disk Radius ◽  
X Ray ◽  
Upper Limit ◽  
Inner Radius ◽  
The Standard Model ◽  
Standard Disk

Abstract We report the serendipitous discovery of a transient X-ray source, Suzaku J1305−4930, ∼3 kpc southwest of the nucleus of the Seyfert 2 galaxy NGC 4945. Among the seven Suzaku observations of NGC 4945 from 2005 to 2011, Suzaku J1305−4930 was detected four times in July and August in 2010. The X-ray spectra are better approximated with a multi-color disk model than a power-law model. At the first detection on 2010 July 4–5, its X-ray luminosity was $(8.9^{+0.2}_{-0.4}) \times 10^{38}\:$erg s−1 and the temperature at the inner-disk radius (kTin) was 1.12 ± 0.04 keV. At the last detection with Suzaku on 2010 August 4–5, the luminosity decreased to $(2.2^{+0.3}_{-0.8}) \times 10^{38}\:$erg s−1 and kTin was 0.62 ± 0.07 keV. The source was not detected on 2011 January 29, about six months after the first detection, with a luminosity upper limit of 2.4 × 1038 erg s−1. We also find an absorption feature which is similar to that reported in Cyg X-1. Assuming the standard disk, we suggest that Suzaku J1305−4930 consists of a black hole with a mass of ∼10 $M_\odot$. The relation between the disk luminosity and kTin is not reproduced with the standard model of a constant inner radius but is better approximated with a slim-disk model.

scholarly journals Measuring the distance to the black hole candidate X-ray binary MAXI J1348–630 using H i absorption

2020 ◽  
Vol 501 (1) ◽  
pp. L60-L64
Author(s):  
J Chauhan ◽  
J C A Miller-Jones ◽  
W Raja ◽  
J R Allison ◽  
P F L Jacob ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutral Hydrogen ◽  
Tangent Point ◽  
X Ray ◽  
Black Hole Candidate ◽  
Upper Limit ◽  
Local Standard ◽  
Point Distance ◽  
Spectral State ◽  
Local Standard Of Rest

ABSTRACT We present neutral hydrogen (H i) absorption spectra of the black hole candidate X-ray binary (XRB) MAXI J1348–630 using the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. The ASKAP H i spectrum shows a maximum negative radial velocity (with respect to the local standard of rest) of −31 ± 4 km s−1 for MAXI J1348–630, as compared to −50 ± 4 km s−1 for a stacked spectrum of several nearby extragalactic sources. This implies a most probable distance of $2.2^{+0.5}_{-0.6}$ kpc for MAXI J1348–630, and a strong upper limit of the tangent point distance at 5.3 ± 0.1 kpc. Our preferred distance implies that MAXI J1348–630 reached 17 ± 10  per cent of the Eddington luminosity at the peak of its outburst, and that the source transited from the soft to the hard X-ray spectral state at 2.5 ± 1.5  per cent of the Eddington luminosity. The MeerKAT H i spectrum of MAXI J1348–630 (obtained from the older, low-resolution 4k mode) is consistent with the re-binned ASKAP spectrum, highlighting the potential of the eventual capabilities of MeerKAT for XRB spectral line studies.

scholarly journals Possible ∼0.4 h X-ray quasi-periodicity from an ultrasoft active galactic nucleus

2020 ◽  
Vol 644 ◽  
pp. L9
Author(s):  
J. R. Song ◽  
X. W. Shu ◽  
L. M. Sun ◽  
Y. Q. Xue ◽  
C. Jin ◽  
...  
Keyword(s):  
Black Hole ◽  
Active Galactic Nucleus ◽  
Quiescent State ◽  
Black Hole Mass ◽  
Resonance Model ◽  
X Ray ◽  
Galactic Black Hole ◽  
Independent Observations ◽  
Extreme Variability ◽  
X Ray Binaries

RX J1301.9+2747 is an ultrasoft active galactic nucleus (AGN) with unusual X-ray variability that is characterized by a long quiescent state and a short-lived flare state. The X-ray flares are found to recur quasi-periodically on a timescale of 13−20 ks. Here, we report the analysis of the light curve in the quiescent state from two XMM-Newton observations spanning 18.5 years, along with the discovery of a possible quasi-periodic X-ray oscillation (QPO) with a period of ∼1500 s. The QPO is detected at the same frequency in the two independent observations, with a combined significance of > 99.89%. The QPO is in agreement with the relation between frequency and black hole mass (MBH) that has been reported in previous works for AGNs and Galactic black hole X-ray binaries (XRBs). The QPO frequency is stable over almost two decades, suggesting that it may correspond to the high-frequency type found in XRBs and originates, perhaps, from a certain disk resonance mode. In the 3:2 twin-frequency resonance model, our best estimate on the MBH range implies that a maximal black hole spin can be ruled out. We find that all ultrasoft AGNs reported so far display quasi-periodicities in the X-ray emission, suggesting a possible link on the part of the extreme variability phenomenon to the ultrasoft X-ray component. This indicates that ultrasoft AGNs could be the most promising candidates in future searches for X-ray periodicities.

Sign in / Sign up

Export Citation Format

Share Document