The SAGE photometric survey: technical description

Abstract

To investigate a huge sample of data related to the Stellar Abundance and Galactic Evolution (SAGE) survey in more detail, we are performing a northern sky photometric survey named SAGES with the SAGE photometric system. This system consists of eight filters: Strömgren-u, SAGE-v, SDSS g, r, i, DDO-51, Hα wide and Hα narrow , including three Sloan broadband filters, three intermediateband filters, two narrow-band filters and one newly-designed narrow-band filter. SAGES covers ∼12 000 square degrees of the northern sky with δ > −5 • , excluding the Galactic disk (|b| < 10 • ) and the sky area 12 h <RA <18 h. The photometric detection limit depth at signal-to-noise ratio 5σ can be as deep as V ∼20 mag. SAGES will produce a photometric catalog with uniform depth for ∼500 million stars with atmospheric parameters including effective temperature T eff , surface gravity log g and metallicity [Fe/H], as well as interstellar extinction to each individual target. In this work, we will briefly introduce the SAGE photometric system, the SAGE survey and a preliminary test field of the open cluster NGC 6791 and its surroundings.

J-PLUS: Stellar parameters, C, N, Mg, Ca, and [α/Fe] abundances for two million stars from DR1

“…Currently, a number of large-scale photometric surveys, for example, the SkyMapper Southern Survey (SMSS): DR1.1 - Wolf et al 2018, DR2 -Onken et al 2019, the Stellar Abundance and Galactic Evolution (SAGE): Zheng et al 2018, the Javalambre Physics of the accelerating universe Astrophysical Survey (J-PAS): Benitez et al 2014, J-PLUS: Cenarro et al 2019, and the Southern Photometric Local Universe Survey (S-PLUS): Mendes de Oliveira et al 2019 are producing huge amounts of valuable photometric data for tens of millions of astronomical objects. The medium-and narrow-band filters of these photometric surveys are designed and optimized for precision measurements of key stellar features, opening up a new era of precise and accurate stellar label determinations (see, e.g., Bailer-Jones 2002;Árnadóttir et al 2010).…”

Comparisons of Different Fitting Methods for the Physical Parameters of A Star Cluster Sample of M33 with Spectroscopy and Photometry

“…As mentioned in Sect. 1, the SAGE survey 5 (PI: Gang Zhao , see, e.g., Fan et al 2018;Zheng et al 2018Zheng et al , 2019a has been operating since 2015 and it covers 12,000 deg 2 of the northern sky with declination δ > −5 • , excluding the Galactic disk (|b| < 10 • ) which is bright and with high extinction. The survey provides photometry in eight bands u SC ,v SAGE , g, r, i, Hα n , Hα w and DDO51.…”

“…The recent SAGE (Stellar Abundances and Galactic Evolution) survey (PI: Gang Zhao , see, e.g., Fan et al 2018;Zheng et al 2018Zheng et al , 2019a covers 12,000 deg 2 of the northern sky with eight photometric bands. Its v SAGE filter is self-designed.…”

Beyond spectroscopy. I. Metallicities, distances, and age estimates for over twenty million stars from SMSS DR2 and Gaia EDR3

“…On the other hand, the large-scale ongoing and planned narrow/medium-bandwidth photometric surveys (see Table 1 for details), such as the SkyMapper Southern Survey (SMSS; Wolf et al 2018), the Pristine survey (Starkenburg et al 2017), the Stellar Abundance and Galactic Evolution survey (SAGE; Zheng et al 2018), the Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS; Benitez et al 2014), the Javalambre/Southern Photometric Local Universe Survey (J/S-PLUS; Cenarro et al 2019; Mendes de Oliveira 2019), and the Multi-channel Photometric Survey Telescope (Mephisto; Er et al, in prep. ), provide a new way to alleviate the target-selection bias and sparse sampling issues of the current large-scale Galactic spectroscopic surveys.…”