AGN feedback in action: a new powerful wind in 1SXPS J050819.8+172149?

Ballo, L.; Severgnini, P.; Braito, V.; Campana, S.; Ceca, R. Della; Moretti, A.; Vignali, C.

doi:10.1051/0004-6361/201526571

Cited by 9 publications

(5 citation statements)

References 63 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…At the end of this obscured phase, massive quasar-driven outflows blow away most of the cold gas reservoir, creating a population of "red-and-dead" gas-poor elliptical galaxies (e.g., Cattaneo et al 2009). Support for this picture -at least for the most luminous AGN -comes from observations of kpc-scale outflows of molecular gas (e.g., Feruglio et al 2010;Sturm et al 2011;Veilleux et al 2013;Cicone et al 2014), as well as of neutral and ionized gas (e.g., Nesvadba et al 2008;Alexander et aloutflows (UFOs, with velocities typically up to 0.1-0.4c) have been clearly detected in X-rays in a sizable sample of AGN at low redshift (e.g., Reeves et al 2003;Pounds et al 2003;Tombesi et al 2010Tombesi et al , 2012aTombesi et al , 2014Tombesi et al , 2015Giustini et al 2011;Patrick et al 2012;Gofford et al 2013Gofford et al , 2015King et al 2014;Nardini et al 2015;Ballo et al 2015; see also Cappi 2006 for an early review; and Fabian 2012 for a more recent one) and also in a limited number of high-redshift quasars (e.g., Chartas et al 2002Chartas et al , 2007Chartas et al , 2009Chartas et al , 2014Saez et al 2009;Lanzuisi et al 2012). Although original claims of blueshifted absorption features were strongly debated (see Vaughan & Uttley 2008), recent high photon statistics in X-ray spectra of both radio-quiet (e.g., Tombesi et al 2010Tombesi et al , 2011Tombesi et al , 2012aGofford et al 2013) and radio-loud AGN (e.g., Gofford et al 2013;Tombesi et al 2014) have undoubtedly shown that these outflows are not ra...…”

Section: Introductionmentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v > ∼ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N H ≈ 2 × 10 23 cm −2 ), intrinsically luminous (L 2−10 keV ≈ 4 × 10 44 erg s −1 ) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2−3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of 0.14 +0.02 −0.06 c, as derived from photoionization models. The mass outflow rate -∼2 M yr −1 -is similar to the source accretion rate, and the derived mechanical energy rate is ∼9.5 × 10 44 erg s −1 , corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.

show abstract

Section: Introductionmentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The system is at an early stage of merger (11.3 kpc distance) and is known to host an AGN that has optically been classified as Seyfert 2 plus a normal galaxy. The AGN, which is also the component in the system that displays water maser emission, hosts a molecular outflow and probably also a disc wind (Yamashita et al 2017;Ballo et al 2015). NGC 3783 is one of the most intensively monitored Seyfert galaxy at high energies.…”

Section: Appendix B: Maser Typesmentioning

confidence: 99%

Water maser emission in hard X-ray selected AGN

et al. 2017

View full text Add to dashboard Cite

Context. Water megamaser emission at 22 GHz has proven to be a powerful tool for astrophysical studies of active galactic nuclei (AGN) because it allows an accurate determination of the mass of the central black hole and of the accretion disc geometry and dynamics. However, after searches among thousands of galaxies, only about 200 of them have shown such spectroscopic features, most of them of uncertain classification. In addition, the physical and geometrical conditions under which a maser activates are still unknown. Aims. We characterize the occurrence of water maser emission in an unbiased sample of AGN by investigating the relation with the X-ray properties and the possible favourable geometry that is required to detect water maser. Methods. We searched for 22 GHz maser emission in a hard X-ray selected sample of AGN, taken from the INTEGRAL/IBIS survey above 20 keV. Only half of the 380 sources in the sample have water maser data. We also considered a volume-limited sub-sample of 87 sources, for which we obtained new observations with the Green Bank and Effelsberg telescopes (for 35 sources). We detected one new maser and increased its radio coverage to 75%. Results. The detection rate of water maser emission in the total sample is 15±3%. This fraction increases to 19±5% for the complete sub-sample, especially when we consider type 2 (22±5% and 31±10% for the total and complete samples, respectively) and Comptonthick AGN (56±18% and 50±35% for the total and complete samples, respectively). No correlation is found between water maser and X-ray luminosity. We note that all types of masers (disc and jet) are associated with hard X-ray selected AGN.Conclusions. These results demonstrate that the hard X-ray selection may significantly enhance the maser detection efficiency over comparably large optical or infrared surveys. A possible decline in detection fraction with increasing luminosity might suggest that an extremely luminous nuclear environment does not favour maser emission. The large fraction of CT AGN with water maser emission could be explained in terms of geometrical effects. The maser medium would then be the very edge-on portion of the obscuring medium.

show abstract

“…2), characterized by a low outflow velocity (v out ∼ 100−1000 km s −1 ), are found in about 65% of the soft X-ray (E 2 keV) spectra of nearby AGN, and they are often known as warm absorbers (WAs, e.g., Halpern 1984;Blustin et al 2005;McKernan et al 2007;Laha et al 2014). More than 30% of the X-ray detected AGN show evidence of ultra-fast outflows (UFOs, e.g., Chartas et al 2002;Pounds et al 2003a,b;Braito et al 2007;Tombesi et al 2010Tombesi et al , 2015Gofford et al 2013;Nardini et al 2015;Ballo et al 2015). UFOs are extremely highly ionized (log(ξ/erg cm s −1 ) ∼ 3−6) absorbers that are detected as blueshifted absorption lines of Fe XXV and XXVI, with typical outflow velocity of v out ∼ 0.1c, but are capable of reaching near-relativistic values of ∼0.5c (e.g., Reeves et al 2018;Luminari et al 2021).…”

Section: Introductionmentioning

confidence: 99%

X-ray obscuration from a variable ionized absorber in PG 1114+445

Serafinelli

Braito²,

Severgnini³

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Photoionized absorbers of outflowing gas are commonly found in the X-ray spectra of active galactic nuclei. While most of these absorbers are seldom significantly variable, some ionized obscurers have increasingly been found to substantially change their column density on a wide range of timescales. These NH variations are often considered as the signature of the clumpy nature of the absorbers. Here we present the analysis of a new Neil Gehrels Swift Observatory campaign of the type 1 quasar PG 1114+445, which was observed to investigate the time evolution of the multiphase outflowing absorbers previously detected in its spectra. The analyzed dataset consists of 22 observations with a total exposure of ∼90 ks that spans about 20 months. For the whole campaign, we report an unusually low flux state with respect to all previous X-ray observations of this quasar. From the analysis of the stacked spectra, we find a fully covering absorber with a column density log(NH/cm−2) = 22.9−0.1+0.3. This is an order of magnitude higher than the column density measured in the previous observations. This is either due to a variation of the known absorbers or to a new one that eclipses the X-ray emitting source. We also find an ionization parameter of log(ξ/erg cm s−1) = 1.4−0.2+0.6. Assuming that the obscuration lasts for the whole duration of the campaign, that is, more than 20 months, we estimate the minimum distance of the ionized clump, which is located at r ≳ 0.5 pc.

show abstract

AGN feedback in action: a new powerful wind in 1SXPS J050819.8+172149?

Cited by 9 publications

References 63 publications

The XMM deep survey in the CDF-S

The XMM deep survey in the CDF-S

Water maser emission in hard X-ray selected AGN

X-ray obscuration from a variable ionized absorber in PG 1114+445

Contact Info

Product

Resources

About