2022A&A...657A..77W


Query : 2022A&A...657A..77W

2022A&A...657A..77W - Astronomy and Astrophysics, volume 657A, 77-77 (2022/1-1)

Transient obscuration event captured in NGC 3227. II. Warm absorbers and obscuration events in archival XMM-Newton and NuSTAR observations.

WANG Y., KAASTRA J., MEHDIPOUR M., MAO J., COSTANTINI E., KRISS G.A., PINTO C., PONTI G., BEHAR E., BIANCHI S., BRANDUARDI-RAYMONT G., DE MARCO B., GRAFTON-WATERS S., PETRUCCI P.-O., EBRERO J., WALTON D.J., KASPI S., XUE Y., PALTANI S., DI GESU L. and HE Z.

Abstract (from CDS):

The relationship between warm absorber (WA) outflows of active galactic nuclei and nuclear obscuration activities caused by optically thick clouds (obscurers) crossing the line of sight is still unclear. NGC 3227 is a suitable target for studying the properties of both WAs and obscurers because it matches the following selection criteria: WAs in both ultraviolet (UV) and X-rays, suitably variable, bright in UV and X-rays, and adequate archival spectra for making comparisons with the obscured spectra. In the aim of investigating WAs and obscurers of NGC 3227 in detail, we used a broadband spectral-energy-distribution model that is built in findings of the first paper in our series together with the photoionization code of SPEX software to fit the archival observational data taken by XMM-Newton and NuSTAR in 2006 and 2016. Using unobscured observations, we find four WA components with different ionization states (log ξ [erg.cm/s] ∼ -1.0, 2.0, 2.5, 3.0). The highest-ionization WA component has a much higher hydrogen column density (∼1022 cm–2) than the other three components (∼1021 cm–2). The outflow velocities of these WAs range from 100 to 1300 km/s, and show a positive correlation with the ionization parameter. These WA components are estimated to be distributed from the outer region of the broad line region (BLR) to the narrow line region. It is worth noting that we find an X-ray obscuration event in the beginning of the 2006 observation, which was missed by previous studies. We find that it can be explained by a single obscurer component. We also study the previously published obscuration event captured in one observation in 2016, which needs two obscurer components to fit the spectrum. A high-ionization obscurer component (log ξ ∼ 2.80; covering factor Cf ∼ 30%) only appears in the 2016 observation, which has a high column density (∼1023 cm–2). A low-ionization obscurer component (log ξ ∼ 1.0 - 1.9; Cf ∼ 20%-50%) exists in both 2006 and 2016 observations, which has a lower column density (∼1022 cm–2). These obscurer components are estimated to reside within the BLR by their crossing time of transverse motions. The obscurers of NGC 3227 are closer to the center and have larger number densities than the WAs, which indicate that the WAs and obscurers might have different origins.

Abstract Copyright: © ESO 2022

Journal keyword(s): X-rays: galaxies - galaxies: active - galaxies: Seyfert - galaxies: individual: NGC 3227 - techniques: spectroscopic

Simbad objects: 6

goto Full paper

goto View the references in ADS

Number of rows : 6
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 Mrk 335 Sy1 00 06 19.5372339024 +20 12 10.617404076   14.19 13.85     ~ 1203 0
2 NGC 985 Sy1 02 34 37.882 -08 47 17.02   14.64 14.28 12.9   ~ 387 0
3 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1686 2
4 NGC 3227 GiP 10 23 30.5765149296 +19 51 54.282206700   12.61 11.79     ~ 1643 1
5 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1586 0
6 NGC 5548 Sy1 14 17 59.5400291832 +25 08 12.603122268   14.35 13.73     ~ 2589 0

To bookmark this query, right click on this link: simbad:objects in 2022A&A...657A..77W and select 'bookmark this link' or equivalent in the popup menu


2023.01.31-02:15:53

© Université de Strasbourg/CNRS

    • Contact