ATTENZIONE! IL REPOSITORY E’ APERTO ESCLUSIVAMENTE ALL’IMMISSIONE DEI RAPPORTI TECNICI (COLLEZIONE 4.01). NON E’ POSSIBILE INSERIRE PRODOTTI IN TUTTE LE ALTRE COLLEZIONI, A CAUSA DI PROBLEMI TECNICI. THE REPOSITORY IS OPEN EXCLUSIVELY FOR THE SUBMISSION OF TECHNICAL REPORTS (COLLECTION 4.01). SUBMISSIONS TO ALL OTHER COLLECTIONS ARE TEMPORARILY UNAVAILABLE, DUE TO TECHNICAL ISSUES.
 

The nature of the broadband X-ray variability in the dwarf Seyfert galaxy NGC 4395

Journal
Date Issued
2019
Author(s)
Kammoun, ES
•
•
Zoghbi, A
•
Miller, JM
•
Cackett, EM
•
Gallo, E
•
Reynolds, MT
•
Risaliti, G
•
Barret, D
•
Brandt, WN
•
Brenneman, LW
•
Kaastra, JS
•
Koss, M
•
Lohfink, AM
•
Mushotzky, RF
•
Raymond, J
•
Stern, D
DOI
Abstract
We present a flux-resolved X-ray analysis of the dwarf Seyfert 1.8 galaxy NGC 4395, based on three archival XMM-Newton and one archival NuSTAR observations. The source is known to harbor a low-mass black hole (∼ 104-afew× 105M) and shows strong variability in the full X-ray range during these observations. We model the flux-resolved spectra of the source assuming three absorbing layers: neutral, mildly ionized, and highly ionized (NH∼ 1.6× 1022- 3.4× 1023cm-2∼ 0.8-7.8×1022cm-2, and 3.8 × 1022 cm-2, respectively). The source also shows intrinsic variability by a factor of ∼3 on short timescales, which is due to changes in the nuclear flux, assumed to be a power law (Γ = 1.6-1.67). Our results show a positive correlation between the intrinsic flux and the absorbers' ionization parameter. The covering fraction of the neutral absorber varies during the first XMM-Newton observation, which could explain the pronounced soft X-ray variability. However, the source remains fully covered by this layer during the other two observations, largely suppressing the soft X-ray variability. This suggests an inhomogeneous and layered structure in the broad-line region. We also find a difference in the characteristic timescale of the power spectra between different energy ranges and observations. We finally show simulated spectra with XRISM, eXTP, and Athena, which will allow us to characterize the different absorbers, study their dynamics, and will help us identify their locations and sizes.
Volume
886
Issue
2
Start page
145
Uri
Url
Issn Identifier
0004-637X
Ads BibCode
2019ApJ...886..145K
Rights
open.access
File(s)
Loading...
Thumbnail Image
Name

Kammoun_2019_ApJ_886_145.pdf

Description
Pdf editoriale
Size

2.44 MB

Format

Adobe PDF

Checksum (MD5)

28dbc16cefe14e68e963e63a48096881

Loading...
Thumbnail Image
Name

1910.11317.pdf

Description
preprint
Size

1.45 MB

Format

Adobe PDF

Checksum (MD5)

9f45e5d02b5e23204b1dfc8e1cf15d9f