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PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy

  • Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić

Lovro Palaversa et al 2025 The Astronomical Journal 169 .

  • Provider: AAS Journals

Caption: Figure 1.

An illustration of multiple stellar populations. The left panel is a color–magnitude diagram for 841,000 stars from the SDSS Stripe 82 Standard Star Catalog (variable sources are excluded; K. Thanjavur et al. 2021) that have Gaia matches within 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15 (after correcting for proper motion using Gaia measurements). A subset of 415,000 stars with r < 22 and u < 22 are overplotted as blue dots, and 409,000 of those that also have 0.2 < g − i < 3.5 (dominated by main-sequence stars and red giants) are overplotted as cyan dots. Finally, 63,000 stars that have a signal-to-noise ratio for Gaia's parallax measurements of at least 20 are shown as green dots (these stars can be used for the calibration of luminosity–color relations). The same symbol color scheme is used in the other two panels. The three yellow lines in the middle panel show the stellar locus parameterization used by G. M. Green et al. (2014) for three values of metallicity (left to right): [Fe/H] = −2, −1, and 0. In the right panel, the impact of metallicity on the color–color tracks is negligible and all three are indistinguishable from each other. In the bottom of the middle panel, at −0.5 < g − r < 0, the three dark blue sequences correspond to (from left to right) He WDs, H WDs, and BHB stars. The clouds of pale blue dots visible above the main stellar locus in the middle and right panels correspond to unresolved binary stars (V. Smolčić et al. 2004).

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