Repository logo
  • English
  • Italiano
Log In
Have you forgotten your password?
  1. Home
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
  5. The outermost stellar halo of NGC 5128 (Centaurus A): Radial structure
 

The outermost stellar halo of NGC 5128 (Centaurus A): Radial structure

Journal
ASTRONOMY & ASTROPHYSICS  
Date Issued
2022
Author(s)
Rejkuba, M.
•
Harris, W. E.
•
GREGGIO, Laura  
•
Crnojević, D.
•
Harris, G. L. H.
DOI
10.1051/0004-6361/202141347
Abstract
The extended stellar halos of galaxies contain important clues for investigating their assembly history and evolution. We investigate the resolved stellar content and the extended halo of NGC 5128 as a function of galactocentric distance. We used HST images to resolve individual red giant branch (RGB) stars in 28 independent pointings. Star counts from deep VI color-magnitude diagrams reaching at least 1.5 mag below the tip of the RGB are used to derive the surface density distribution of the halo. The contamination by Milky Way stars is assessed with a new control field, with models, and by combining optical and near-IR photometry. We present a new calibration of the WFC3 F606W+F814W photometry to the ground-based VI photometric system. The photometry shows that the stellar halo of NGC 5128 is dominated by old RGB stars that are present in all fields. The V-band surface brightness changes from 23 to 32 mag/arcsec$^2$ between 8.3 kpc from the galaxy center to our outermost halo fields located 140 kpc away from the center along the major axis and 92 kpc along the minor axis. Within ~30 kpc, we also find evidence for a 2-3 Gyr old population traced by bright asymptotic giant branch stars. This population contributes only up to 10% in total stellar mass if it is 2 Gyr old, but a larger fraction of 30-40% is required if its age is 3 Gyr. The stellar surface density profile is well fit by a r$^{1/4}$ curve or a power-law $\sim r^{-3.1}$ over the full radial range, with no obvious break in the slope, but with large field-to-field scatter. The ellipticity measured from integrated-light photometry in the inner parts, $e=(b/a)=0.77$, flattens to $e=0.54 \pm 0.02$ beyond 30 kpc. Considering the flattening of the outer halo, the projection of the elliptical isophote on the semimajor axis for our most distant field reaches nearly 30 effective radii. [abridged]
Volume
657
Start page
A41
Uri
http://hdl.handle.net/20.500.12386/32329
Url
https://www.aanda.org/articles/aa/full_html/2022/01/aa41347-21/aa41347-21.html
http://arxiv.org/abs/2111.02945v1
Issn Identifier
0004-6361
Ads BibCode
2022A&A...657A..41R
Rights
open.access
File(s)
Loading...
Thumbnail Image
Name

cena_pap3A.pdf

Description
PDF editoriale
Size

2.74 MB

Format

Adobe PDF

Checksum (MD5)

c3a86c89a72bb5d8d72fcace137aa32c

Explore By
  • Communities and Collection
  • Research Outputs
  • Researchers
  • Organizations
  • Projects
Information and guides for authors
  • https://openaccess-info.inaf.it: all about open access in INAF
  • How to enter a product: guides to OA@INAF
  • The INAF Policy on Open Access
  • Downloadable documents and templates

Built with DSpace-CRIS software - Extension maintained and optimized by 4Science

  • Privacy policy
  • End User Agreement
  • Send Feedback