Multicolor Optical Monitoring of the Quasar 3C 273 from 2005 to 2016

Xiong, Dingrong; Bai, J. M.; Zhang, Haojing; Fan, J. H.; Gu, Minfeng; Yi, Ting-Feng; Zhang, Xiong

doi:10.3847/1538-4365/aa64d2

Cited by 55 publications

(75 citation statements)

References 113 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This includes NLS1 AGNs Mkn 335 (e.g., Grupe et al 2007) and 1H 0707-495 (e.g., Boller et al 2002); one of the least luminous, lowest mass and nearest Seyfert 1 Galaxy NGC4395 (Filippenko & Ho 2003) which has also been classified as a BLS1/S1.9 (Nikołajuk et al 2009), and CGCG 229-10 also called Zw 299-015 which is a Type I Seyfert Galaxy that exhibits broad-line emission (e.g., Barth et al 2011). In addition to these four we also included broad-line Seyfert 1.5 AGN NGC 3227 (see e.g., Markowitz et al 2009, and references therein), high frequency BL Lac blazar PKS 2155-304 (e.g., Zhang et al 1999Zhang et al , 2005, optically violent variable blazars 3c279 (e.g., Hartman et al 1996;Chatterjee et al 2008) and 3c345 (e.g., Kidger & de Diego 1990), and quasars 3c454.3 (e.g., Fuhrmann et al 2006;Giommi et al 2006) and 3c273 (e.g., Kaastra & Roos 1992;Xiong et al 2017). These sources are optimal for our analysis as they have a sufficiently large number of observations such that the emission from these events has a temporal coverage similar to those seen for our TDE sample.…”

Section: Brightness As a Function Of Redshiftmentioning

confidence: 99%

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Auchettl

Ramírez-Ruiz

Guillochon

2018

ApJ

View full text Add to dashboard Cite

One of the main challenges of current tidal disruption events (TDEs) studies is that emission arising from AGN activity may potentially mimic the expected X-ray emission of a TDE. Here we compare the X-ray properties of TDEs and AGN to determine a set of characteristics which would allow us to discriminate between flares arising from these two objects. We find that at peak, TDEs are brighter than AGN found at similar redshifts. However, compared to preflare upperlimits, highly variable AGN can produce flares of a similar order of magnitude as those seen from X-ray TDEs. Nevertheless, TDEs decay significantly more monotonically, and their emission exhibits little variation in spectral hardness as a function of time. We also find that X-ray TDEs are less absorbed, and their emission is much softer than the emission detected from AGN found at similar redshifts. We derive the X-ray luminosity function (LF) for X-ray TDEs using the events from Auchettl et al. (2017). Interestingly, our X-ray LF matches closely the theoretically derived LF by Milosavljević et al. (2006) which assumes a higher TDE rate currently estimated from observations. Using our results and the results of Stone & Metzger (2016), we estimate a TDE rate of (0.7 − 4.7) × 10 −4 yr −1 per galaxy, higher than current observational estimates. We find that TDEs can contribute significantly to the LF of AGN for z 0.4, while there is no evidence that TDEs influence the growth of 10 6−7 M BHs. However, BHs < 10 6 M can grow from TDEs arising from super-Eddington accretion without contributing significantly to the observed AGN LF at z = 0.

show abstract

Section: Brightness As a Function Of Redshiftmentioning

confidence: 99%

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Auchettl

Ramírez-Ruiz

Guillochon

2018

ApJ

View full text Add to dashboard Cite

show abstract

“…After 2012, the filters of 60 cm optical telescope were changed into ugri of SDSS. Further details about the three telescopes are seen in Liao et al (2014), Xiong et al (2017) and Hong et al (2017). In this work, S5 0716+714 is observed with 2.4 m and 1.02 m telescopes.…”

Section: Observations and Data Reductionmentioning

confidence: 62%

“…The specific formulas and variability criterion about the two statistical techniques are seen in these references (e.g., de Diego 2010;Goyal et al 2012;Hu et al 2014;Agarwal & Gupta 2015;Dai et al 2015;Xiong et al 2016Xiong et al , 2017Hong et al 2017). The BL Lac object is considered as variability (V) if the light curve satisfies the two criteria of F -test and ANOVA, probably variable (PV) if only one of the above two criteria is satisfied, and non-variable (N) if none of the criteria are met.…”

Section: Resultsmentioning

confidence: 99%

“…In order to explore mechanism of variability, we monitored many radio loud AGNs using the 2.4 m, 1.02 m and 60 cm optical telescopes located at the Yunnan Astronomical Observatories (YAO) of Chinese Academy of Sciences of China from 2005 to 2012 (e.g., Liao -5 -et al 2014;Xiong et al 2016Xiong et al , 2017Wang et al 2017;Guo et al 2017;Hong et al 2017).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

See 1 more Smart Citation

Optical Quasi-periodic Oscillation of the BL Lacertae Object S5 0716+714 during the Faint State

Hong

Xiong

Bai

2017

Self Cite

View full text Add to dashboard Cite

“…Presently, a number of statistical tests, such as the C-test, the F-test, the χ 2 -test and one-way analysis of variance (ANOVA), have been proposed to assess quantitatively whether there are IDVs [6,9,[19][20][21][22][23]. Here, we apply the F-test and χ 2 -test to cross-check the intra-day light curves.…”

Section: Variabilitymentioning

confidence: 99%

Intra-Night Variability of OJ 287 with Long-Term Multiband Optical Monitoring

Zeng

Zhao²,

Jiang

et al. 2017

Galaxies

View full text Add to dashboard Cite

Abstract:We present long-term optical multi-band photometric monitoring of the blazar OJ 287 from 6 March 2010 to 3 April 2016, with high temporal resolution in the VRI-bands. The flux variations and colour-magnitude variations on long and short timescales were investigated to understand the emission mechanisms. In our observation, the major outbursts occurred in January 2016, as predicted by the binary pair of black holes model for OJ 287, with F var of 1.3∼2.1%, and variability amplitude (Amp) of 5.8∼9.0%. The intra-night variability (IDV) durations were from 18.5 to 51.3 min, and the minimal variability timescale was about 4.7 min. The colour-magnitude variation showed a weak positive correlation on the long timescale with Pearson's r = 0.450, while a negative correlation was found on intra-night timescales. We briefly discuss the possible physical mechanisms that are most likely to be responsible for the observed flux and colour-magnitude correlation variability.

show abstract

Multicolor Optical Monitoring of the Quasar 3C 273 from 2005 to 2016

Cited by 55 publications

References 113 publications

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Optical Quasi-periodic Oscillation of the BL Lacertae Object S5 0716+714 during the Faint State

Intra-Night Variability of OJ 287 with Long-Term Multiband Optical Monitoring

Contact Info

Product

Resources

About