The dark matter halo masses of elliptical galaxies as a function of observationally robust quantities

Journal Article · Tue Jun 14 00:00:00 EDT 2022 · Astronomy and Astrophysics

DOI:https://doi.org/10.1051/0004-6361/202142511· OSTI ID:1982320

Sonnenfeld, Alessandro ^[1]; Tortora, Crescenzo ^[2]; Hoekstra, Henk ^[1]; Asgari, Marika ^[3]; Bilicki, Maciej ^[4]; Heymans, Catherine ^[5]; Hildebrandt, Hendrik ^[6]; Kuijken, Konrad ^[1]; Napolitano, Nicola R. ^[7]; Roy, Nivya ^[8]; Valentijn, Edwin ^[9]; Wright, Angus H. ^[6]

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1. Leiden Univ. (Netherlands). Leiden Observatory
2. Istituto Nazionale di Astrofisica (INAF), Naples (Italy). Osservatorio Astronomico di Capodimonte
3. Univ. of Edinburgh, Scotland (United Kingdom). The Royal Observatory; University of Hull (United Kingdom). E.A. Milne Centre
4. Polish Academy of Sciences (PAS), Warsaw (Poland). Center for Theoretical Physics
5. Univ. of Edinburgh, Scotland (United Kingdom). The Royal Observatory; Ruhr Univ., Bochum (Germany)
6. Ruhr Univ., Bochum (Germany)
7. Sun Yat-Sen Univ., Guangzhou (China); CSST Science Center for Guangdong-Hong Kong-Macau Great Bay Area, Zhuhai (China)
8. Carmel College, Mala (India)
9. Univ. of Groningen (Netherlands)

Context. The assembly history of the stellar component of a massive elliptical galaxy is closely related to that of its dark matter halo. Measuring how the properties of galaxies correlate with their halo mass can therefore help to understand their evolution. Aims. We investigate how the dark matter halo mass of elliptical galaxies varies as a function of their properties, using weak gravitational lensing observations. To minimise the chances of biases, we focus on the following galaxy properties that can be determined robustly: the surface brightness profile and the colour. Methods. We selected 2409 central massive elliptical galaxies (log M*/M_⊙ ≳ 11.4) from the Sloan Digital Sky Survey spectroscopic sample. We first measured their surface brightness profile and colours by fitting Sérsic models to photometric data from the Kilo-Degree Survey (KiDS). We fitted their halo mass distribution as a function of redshift, rest-frame r-band luminosity, half-light radius, and rest-frame u - g colour, using KiDS weak lensing measurements and a Bayesian hierarchical approach. For the sake of robustness with respect to assumptions on the large-radii behaviour of the surface brightness, we repeated the analysis replacing the total luminosity and half-light radius with the luminosity within a 10 kpc aperture, L_{r, 10}, and the light-weighted surface brightness slope, Γ₁₀. Results. We did not detect any correlation between the halo mass and either the half-light radius or colour at fixed redshift and luminosity. Using the robust surface brightness parameterisation, we found that the halo mass correlates weakly with L_r,10 and anti-correlates with Γ₁₀. At fixed redshift, L_{r, 10} and Γ₁₀, the difference in the average halo mass between galaxies at the 84th percentile and 16th percentile of the colour distribution is 0.00 ± 0.11 dex. Conclusion. Our results indicate that the average star formation efficiency of massive elliptical galaxies has little dependence on their final size or colour. This suggests that the origin of the diversity in the size and colour distribution of these objects lies with properties other than the halo mass.

• Research Organization: US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
• Sponsoring Organization: USDOE
• Contributing Organization: Sloan Digital Sky Survey (SDSS)
• OSTI ID: 1982320
• Journal Information: Astronomy and Astrophysics, Journal Name: Astronomy and Astrophysics Vol. 662; ISSN 0004-6361
• Publisher: EDP Sciences
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
cD
elliptical and lenticular galaxies
fundamental parameters
galaxies
gravitational lensing
weak galaxies