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Cited article:

Extinction Distributions in Nearby Star-resolved Galaxies. I. M31

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Red supergiants in M31: the Humphreys–Davidson limit at high metallicity

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A Sub-2% Distance to M31 from Photometrically Homogeneous Near-infrared Cepheid Period–Luminosity Relations Measured with the Hubble Space Telescope

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The Astrophysical Journal 920 (2) 84 (2021)
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The True Luminosities of Planetary Nebulae in M31's Bulge: Massive Central Stars from an Old Stellar Population

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The Astrophysical Journal 863 (2) 189 (2018)
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Black Holes and Neutron Stars in Nearby Galaxies: Insights from NuSTAR

N. Vulic, A. E. Hornschemeier, D. R. Wik, M. Yukita, A. Zezas, A. F. Ptak, B. D. Lehmer, V. Antoniou, T. J. Maccarone, B. F. Williams and F. M. Fornasini
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Supermassive Black Holes as the Regulators of Star Formation in Central Galaxies

Bryan A. Terrazas, Eric F. Bell, Joanna Woo and Bruno M. B. Henriques
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Stellar kinematics using a third integral of motion: method and application on the Andromeda galaxy

R. Kipper, P. Tenjes, O. Tihhonova, A. Tamm and E. Tempel
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Recovering 3D structural properties of galaxies from SDSS-like photometry

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Balancing mass and momentum in the Local Group

J. D. Diaz, S. E. Koposov, M. Irwin, V. Belokurov and N. W. Evans
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THE SURVEY OF LINES IN M31 (SLIM): INVESTIGATING THE ORIGINS OF [C II] EMISSION

M. J. Kapala, K. Sandstrom, B. Groves, et al.
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The distribution of interstellar dust in CALIFA edge-on galaxies via oligochromatic radiative transfer fitting

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ACTIVE GALACTIC NUCLEUS AND QUASAR SCIENCE WITH APERTURE MASKING INTERFEROMETRY ON THEJAMES WEBB SPACE TELESCOPE

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The Astrophysical Journal 783 (2) 73 (2014)
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Evidence for spin alignment of spiral and elliptical/S0 galaxies in filaments

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THE CLUSTER OF BLUE STARS SURROUNDING THE M31 NUCLEAR BLACK HOLE

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THE STABILITY OF LOW SURFACE BRIGHTNESS DISKS BASED ON MULTI-WAVELENGTH MODELING

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The Astrophysical Journal 741 (1) 6 (2011)
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Stellar Populations in M31 from Broad-band Photometry

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BULGELESS GIANT GALAXIES CHALLENGE OUR PICTURE OF GALAXY FORMATION BY HIERARCHICAL CLUSTERING,

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