Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (12) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· NED Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Infrared Spectroscopy of Pa(Beta) and [Fe II] Emission in NGC 4151
Authors:
Knop, R. A.; Armus, L.; Larkin, J. E.; Mathews, K.; Shupe, D. L.; Soifer, B. T.
Publication:
Astronomical Journal v.112, p.81 (AJ Homepage)
Publication Date:
07/1996
Origin:
AJ
AJ/ApJ Keywords:
GALAXIES: INDIVIDUAL: NGC 4151, GALAXIES: SEYFERT, GALAXIES: NUCLEI
DOI:
10.1086/117990
Bibliographic Code:
1996AJ....112...81K

Abstract

We present spatially resolved 1.24-1.30 micron spectroscopy with a resolution of 240 km/s of the Seyfert 1.5 galaxy NGC 4151. Broad Paβ, narrow Paβ, and narrow [Fe II] (λ = 1.2567 microns) emission lines are identified in the spectrum. Additionally, a spatially unresolved narrow component probably due to [S IX] = (λ = 1.25235 microns) is observed on the nucleus. The narrow Paβ and [Fe II] lines are observed to be extended over a scale of 5". The spatial variation of the velocity centers of the Paβ and [Fe II] lines show remarkable similarity, and additionally show similarities to the velocity structure previously observed in ground based spectroscopy of [O III] emission in NGC 4151. This leads to the conclusion that the [Fe II] emission arises in clouds in the Seyfert narrow line region that are physically correlated with those narrow line clouds responsible for the optical emission. The [Fe II] emission line, however, is significantly wider than the Paβ emission line along the full spatial extent of the observed emission. This result suggests that despite the correlation between the bulk kinematics of Paβ and [Fe II], there is an additional process, perhaps fast shocks from a wind in the Seyfert nucleus, contributing to the [Fe II] emission.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints