Detection of a Compact Nuclear Radio Source in the Local Group Elliptical Galaxy M32

Yang, Yang; Li, Zhiyuan; Sjouwerman, Loránt O.; Wang, Q. Daniel; Gu, Qiusheng; Kraft, Ralph; Yuan, Feng

doi:10.1088/2041-8205/807/1/l19

Cited by 10 publications

(9 citation statements)

References 48 publications

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“…The YC05 predictions have been confirmed by many observational and theoretical works (see review by Yuan & Narayan 2014), both of AGNs (e.g., Pellegrini et al 2007;Wu, Yuan & Ho 2007;Wrobel, Terashima & Ho 2008;Yuan, Yu & Ho 2009, hereafter YYH09;de Gasperin et al 2011;Younes et al 2012;Li, Yuan & Xie 2016) and BHBs (e.g., Pszota et al 2008;Plotkin et al 2013;Reynolds et al 2014;Xie, Yang & Ma 2014;Yang et al 2015a). For example, YYH09 did a statistical analysis based on a sample consisting of 22 quiescent AGNs.…”

Section: Introductionmentioning

confidence: 77%

“…The main improvement to YYH09 is the sample size, which is enlarged from 22 to 75. Besides, the radio emission of several sources, e.g., M31 (Bender et al 2005;Garcia et al 2010, L X ∼ 10 −10.2 L Edd ) and M32 (Yang et al 2015a), is now firmly detected, while in YYH09 their radio emission only has upper limit constraint. The main conclusion remains unchanged, i.e.…”

Section: Yuan Yu and Ho (2009) (Yyh09)mentioning

confidence: 97%

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Fundamental Plane of Black Hole Activity in the Quiescent Regime

Xie

Yuan

2017

ApJ

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A correlation among the radio luminosity (L R ), X-ray luminosity (L X ), and black hole mass (M BH ) in active galactic nuclei (AGNs) and black hole binaries is known to exist and is called the "Fundamental Plane" of black hole activity. predicts that the radio/X-ray correlation index, ξ X , changes from ξ X ≈ 0.6 to ξ X ≈ 1.2 − 1.3 when L X /L Edd decreases below a critical value ∼ 10 −6 . While many works favor such a change, there are also several works claiming the opposite. In this paper, we gather from literature a largest quiescent AGN (defined as L X /L Edd 10 −6 ) sample to date, consisting of 75 sources. We find that these quiescent AGNs follow a ξ X ≈ 1.23 radio/X-ray relationship, in excellent agreement with the Yuan & Cui prediction. The reason for the discrepancy between the present result and some previous works is that their samples contain not only quiescent sources but also "normal" ones (i.e., L X /L Edd 10 −6 ). In this case, the quiescent sources will mix up with those normal ones in L R and L X . The value of ξ X will then be between 0.6 and ∼ 1.3, with the exact value being determined by the sample composition, i.e., the fraction of the quiescent and normal sources. Based on this result, we propose that a more physical way to study the Fundamental Plane is to replace L R and L X with L R /L Edd and L X /L Edd , respectively.

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Section: Introductionmentioning

confidence: 77%

Section: Yuan Yu and Ho (2009) (Yyh09)mentioning

confidence: 97%

Fundamental Plane of Black Hole Activity in the Quiescent Regime

Xie

Yuan

2017

ApJ

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“…For simplicity, we used the HIP 1123 (A1V ) telluric taken with NGC 404 for our flux calibration. We then checked to make sure the photometric calibration did Yang et al (2015) "L" represents LINER,"S" represents Seyfert, "T" represents objects with a LINER + H II type region spectrum, and "A" indicates absorption-line spectrum as detailed in Ho et al (1997). "R" indicates nuclear radio emission, and "RJ" labels radio jet emission as described in Liu & Zhang (2002); Nagar et al (2005).…”

Section: Flux Calibrationmentioning

confidence: 99%

Surprisingly Strong K-band Emission Found in Low-luminosity Active Galactic Nuclei

Dumont

Seth

Strader

et al. 2019

ApJ

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We examine the near-infrared (NIR) emission from low-luminosity AGNs (LLAGNs). Our galaxy sample includes 15 objects with detected 2-10 keV X-ray emission, dynamical black hole mass estimates from the literature, and available Gemini/NIFS integral field spectroscopy (IFU) data. We find evidence for red continuum components at the center of most galaxies, consistent with the hot dust emission seen in higher luminosity AGN. We decompose the spectral data cubes into a stellar and continuum component, assuming the continuum component comes from thermal emission from hot dust. We detect nuclear thermal emission in 14 out of 15 objects. This emission causes weaker CO absorption lines and redder continuum (2.05 − 2.28 µm) in our K-band data, as expected from hot dust around an AGN. The NIR emission is clearly correlated with the 210 keV X-ray flux, with a Spearman coefficient of r spearman = 0.69 suggesting a > 99% significance of correlation, providing further evidence of an AGN origin. Our sample has typical X-ray and NIR fluxes 3 − 4 orders of magnitude less luminous than previous work studying the NIR emission from AGN. We find that the ratio of NIR to X-ray emission increases towards lower Eddington ratios. The NIR emission in our sample is often brighter than the X-ray emission, with our K band AGN luminosities comparable to or greater than the 2-10 keV X-ray luminosities in all objects with Eddington ratios below 0.01%. The nature of this LLAGN NIR emission remains unclear, with one possibility being an increased contribution from jet emission at these low luminosities. These observations suggest JWST will be a useful tool for detecting the lowest luminosity AGN.

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“…Therefore, relativistic electrons should be present in the winds and emit radio emission via synchrotron radiation. Recently, we detected the radio counterpart of the central SMBH in M 32 (named M 32*), a dwarf elliptical companion of M 31, using deep JVLA C-band observations (Yang et al 2015). M 32* has a 6 GHz flux density similar to that of M 31*, and also shows a pc-scale, extended morphology marginally resolved by the synthesized beam.…”

Section: Spectrum and Morphology: Insights On The Putative Jetmentioning

confidence: 99%

Very Large Array Multiband Monitoring Observations of M31*

Yang

Sjouwerman

et al. 2017

ApJ

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The Andromeda galaxy (M 31) hosts one of the nearest and most quiescent super-massive black holes, which provides a rare, but promising opportunity for studying the physics of black hole accretion at the lowest state. We have conducted a multi-frequency, multi-epoch observing campaign, using the Karl G. Jansky Very Large Array (VLA) in its extended configurations in 2011-2012, to advance our knowledge of the still poorly known radio properties of M 31*. For the first time, we detect M 31* at 10, 15 and 20 GHz, and measure its spectral index, α ≈ −0.45 ± 0.08 (S ν ∝ ν α ), over the frequency range of 5-20 GHz. The relatively steep spectrum suggests that the observed radio flux is dominated by the optically-thin part of a putative jet, which is located at no more than a few thousand Schwarzschild radii from the black hole. On the other hand, our sensitive radio images show little evidence for an extended component, perhaps except for several parsec-scale "plumes", the nature of which remains unclear. Our data also reveal significant (a few tens of percent) flux variation of M 31* at 6 GHz, on timescales of hours to days. Furthermore, a curious decrease of the mean flux density, by ∼50%, is found between VLA observations taken during 2002-2005 and our new observations, which might be associated with a substantial increase in the mean X-ray flux of M 31* starting in 2006.

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Detection of a Compact Nuclear Radio Source in the Local Group Elliptical Galaxy M32

Cited by 10 publications

References 48 publications

Fundamental Plane of Black Hole Activity in the Quiescent Regime

Fundamental Plane of Black Hole Activity in the Quiescent Regime

Surprisingly Strong K-band Emission Found in Low-luminosity Active Galactic Nuclei

Very Large Array Multiband Monitoring Observations of M31*

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