NuSTAR observations of water megamaser AGN

Masini, Alberto; Comastri, A.; Baloković, Mislav; Zaw, I.; Puccetti, S.; Ballantyne, D. R.; Bauer, F. E.; Boggs, Steven E.; Brandt, W. N.; Brightman, Murray; Christensen, Finn Erland; Craig, William W.; Gandhi, P.; Hailey, Charles J.; Harrison, Fiona A.; Koss, Michael; Madejski, G. M.; Ricci, Cláudio; Rivers, Elizabeth; Stern, Daniel; Zhang, W. W.

doi:10.1051/0004-6361/201527689

Cited by 78 publications

(115 citation statements)

References 69 publications

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“…The maser activity could indeed be associated with a dusty Keplerian disk orbiting the SMBH, from which the most precise BH mass available to date could be derived (e.g, Kuo et al 2011). This would allow a direct comparison of this object with other samples of disk masers (Pesce et al 2015;Masini et al 2016) and get clues on the Xray absorber. On the other hand, the maser spots could either be associated with the outflow seen in the optical spectrum, invalidating any possible BH mass estimate.…”

Section: Eclipsing Eventmentioning

confidence: 97%

The Phoenix galaxy as seen byNuSTAR

Masini

Comastri

Puccetti

et al. 2017

A&A

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Aims. We study the long-term variability of the well-known Seyfert 2 galaxy Mrk 1210 (a.k.a. UGC 4203, or the Phoenix galaxy). Methods. The source was observed by many X-ray facilities in the last 20 years. Here we present a NuSTAR observation and put the results in context of previously published observations. Results. NuSTAR observed Mrk 1210 in 2012 for 15.4 ks. The source showed Compton-thin obscuration similar to that observed by Chandra, Suzaku, BeppoSAX and XMM-Newton over the past two decades, but different from the first observation by ASCA in 1995, in which the active nucleus was caught in a low flux state -or obscured by Compton-thick matter, with a reflection-dominated spectrum. Thanks to the high-quality hard X-ray spectrum obtained with NuSTAR and exploiting the long-term spectral coverage spanning 16.9 years, we can precisely disentangle the transmission and reflection components and put constraints on both the intrinsic long-term variability and hidden nucleus scenarios. In the former case, the distance between the reflector and the source must be at least ∼ 2 pc, while in the latter one the eclipsing cloud may be identified with a water maser-emitting clump.

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Section: Eclipsing Eventmentioning

confidence: 97%

The Phoenix galaxy as seen byNuSTAR

Masini

Comastri

Puccetti

et al. 2017

A&A

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“…Since the seminal works about clumpy tori (Nenkova et al 2008) there is growing evidence against the monolithic obscurer envisaged by unified models Masini et al 2016;Marinucci et al 2016) of the Compton-thick clouds in the circumnuclear environment of NGC 4945. Fig.…”

Section: Clumpiness Of the Reflectormentioning

confidence: 99%

Spatially resolved Fe K spectroscopy of NGC 4945

Marinucci

Bianchi

Fabbiano

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the imaging and spectroscopic analysis of the combined Chandra ACIS-S observations of the Compton-thick Seyfert 2 galaxy NGC 4945. We performed a spatially-resolved spectroscopy of the circumnuclear environment of the source, picturing the innermost 200 parsecs around the highly absorbed nucleus. The additional 200 ks ACIS-S data with respect to the previous campaign allowed us to map with even greater detail the central structure of this source and to discover an enhanced iron emission in the innermost nuclear region, with respect to the associated Compton reflection continuum. We revealed that the Equivalent Width of the iron Kα line is spatially variable (ranging from 0.5 to 3 keV), on scales of tens of parsecs, likely due to the ionization state and orientation effects of the reprocessing material, with respect to the central X-ray illuminating source. A clump of highly ionized Fe xxv He-α is also detected, 40 parsecs east to the nucleus. When observations taken years apart are considered, the central unresolved reflected emission is found to remain constant.

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“…Because of the 100-fold increase in sensitivity between Swift/BAT and NuSTAR, for any source detected in the Swift/BAT all-sky survey, even a short exposure results in data with signal-to-noise ratio (SNR) high enough for spectral modelling up to ∼70 keV (e.g. Baloković et al 2014;Koss et al 2015;Masini et al 2016).…”

Section: S a M P L E S E L E C T I O Nmentioning

confidence: 99%

The infrared to X-ray correlation spectra of unobscured type 1 active galactic nuclei

García-Bernete¹,

Almeida²,

Landt³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Citation for published item:qr¡ %EferneteD sF nd mos elmeidD gF nd vndtD rF nd rdD wF tF nd flokovi¡ D wF nd eostEulidoD tF eF @PHIUA 9he infrred to Ery orreltion spetr of unosured type I tive glti nuleiF9D wonthly noties of the oyl estronomil oietyFD RTW @IAF ppF IIHEIPTF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe use new X-ray data obtained with the Nuclear Spectroscopic Telescope Array (NuSTAR), near-infrared (NIR) fluxes and mid-infrared (MIR) spectra of a sample of 24 unobscured type 1 active galactic nuclei (AGN) to study the correlation between various hard X-ray bands between 3 and 80 keV and the infrared (IR) emission. The IR to X-ray correlation spectrum (IRXCS) shows a maximum at ∼15-20 µm, coincident with the peak of the AGN contribution to the MIR spectra of the majority of the sample. There is also an NIR correlation peak at ∼2 µm, which we associate with the NIR bump observed in some type 1 AGN at ∼1-5 µm and is likely produced by nuclear hot dust emission. The IRXCS shows practically the same behaviour in all the X-ray bands considered, indicating a common origin for all of them. We finally evaluated correlations between the X-ray luminosities and various MIR emission lines. All the lines show a good correlation with the hard X-rays (ρ ≥ 0.7), but we do not find the expected correlation between their ionization potentials and the strength of the IRXCS.

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NuSTAR observations of water megamaser AGN

Cited by 78 publications

References 69 publications

The Phoenix galaxy as seen byNuSTAR

The Phoenix galaxy as seen byNuSTAR

Spatially resolved Fe K spectroscopy of NGC 4945

The infrared to X-ray correlation spectra of unobscured type 1 active galactic nuclei

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