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  The survey of planetary nebulae in Andromeda (M 31) - II. Age–velocity dispersion relation in the disc from planetary nebulae

Bhattacharya, S., Arnaboldi, M., Caldwell, N., Gerhard, O., Blaña, M., McConnachie, A., et al. (2019). The survey of planetary nebulae in Andromeda (M 31) - II. Age–velocity dispersion relation in the disc from planetary nebulae. Astronomy and Astrophysics, 631: A56. doi:10.1051/0004-6361/201935898.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-4940-0 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-4941-F
Genre: Journal Article

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Bhattacharya, Souradeep, Author
Arnaboldi, Magda, Author
Caldwell, Nelson, Author
Gerhard, Ortwin1, Author              
Blaña, Matias1, Author              
McConnachie, Alan, Author
Hartke, Johanna, Author
Guhathakurta, Puragra, Author
Pulsoni, Claudia1, Author              
Freeman, Kenneth C., Author
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1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Abstract: Context. The age–velocity dispersion relation is an important tool to understand the evolution of the disc of the Andromeda galaxy (M 31) in comparison with the Milky Way. Aims. We use planetary nebulae (PNe) to obtain the age–velocity dispersion relation in different radial bins of the M 31 disc. Methods. We separate the observed PNe sample based on their extinction values into two distinct age populations in the M 31 disc. The observed velocities of our high- and low-extinction PNe, which correspond to higher- and lower-mass progenitors, respectively, are fitted in de-projected elliptical bins to obtain their rotational velocities, Vϕ, and corresponding dispersions, σϕ. We assign ages to the two PN populations by comparing central-star properties of an archival sub-sample of PNe, that have models fitted to their observed spectral features, to stellar evolution tracks. Results. For the high- and low-extinction PNe, we find ages of ∼2.5 and ∼4.5 Gyr, respectively, with distinct kinematics beyond a deprojected radius RGC = 14 kpc. At RGC = 17–20 kpc, which is the equivalent distance in disc scale lengths of the Sun in the Milky Way disc, we obtain σϕ,  2.5 Gyr = 61 ± 14 km s−1 and σϕ,  4.5 Gyr = 101 ± 13 km s−1. The age–velocity dispersion relation for the M 31 disc is obtained in two radial bins, RGC = 14–17 and 17–20 kpc. Conclusions. The high- and low-extinction PNe are associated with the young thin and old thicker disc of M 31, respectively, whose velocity dispersion values increase with age. These values are almost twice and three times that of the Milky Way disc stellar population of corresponding ages, respectively. From comparison with simulations of merging galaxies, we find that the age–velocity dispersion relation in the M 31 disc measured using PNe is indicative of a single major merger that occurred 2.5–4.5 Gyr ago with an estimated merger mass ratio ≈1:5.

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 Dates: 2019-10-21
 Publication Status: Published online
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 Identifiers: DOI: 10.1051/0004-6361/201935898
Other: LOCALID: 3222316
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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
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Publ. Info: France : EDP Sciences S A
Pages: - Volume / Issue: 631 Sequence Number: A56 Start / End Page: - Identifier: ISSN: 1432-0746
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1