2023 SDSS-V Collaboration Meeting

Session

Session 5

Aug 1, 2023, 1:30 PM

Gerald D. Fischbach Auditorium/2-GDFA (160 5th Avenue)

Conveners

Session 5

• Benny Trakhtenbrot

33. Exploring "Changing-look" AGNs: First Results from SDSS-V

Grisha Zeltyn

8/1/23, 1:30 PM

Recent advances in time-domain surveys have revealed dramatic changes to SMBH accretion and AGN appearance on surprisingly short timescales. Among those, changing-look AGNs (CL-AGNs) show the (dis)appearance of broad emission lines and/or the quasar-like continuum, on timescales of years and sometimes even months. These dramatic changes may be driven by significant changes to the accretion...

35. Fast Marginalization Methods for Modern Astronomical Pipelines

Douglas Finkbeiner

8/1/23, 1:42 PM

Spectroscopic data reduction is confounded by unknowns such as the sky spectrum and the instrumental transfer function. It is important to marginalize over these (and not merely subtract a point estimate) in order to obtain unbiased results with correct error bars. When the priors on the nuisance components can be expressed as a Gaussian in the high-dimension pixel space (i.e., an Npix x Npix...

36. A New MWM Pipeline: Separating APOGEE Spectra into Components

Andrew Saydjari

8/1/23, 1:54 PM

A ubiquitous problem in astronomy is correctly assigning absorption or emission features in a spectrum to the multiple processes occurring along the line of sight within the spectroscopic field of view. We introduce a new data processing pipeline to decompose APOGEE spectra into components associated with the target star, terrestrial atmosphere, and dust along the line of sight. In this model,...

86. KPM: A flexible and data-driven K process model for nucleosynthesis

Emily Griffith

8/1/23, 2:06 PM

The element abundance pattern seen in Milky Way disk stars is close to two-dimensional, dominated by production from one prompt process and one delayed process. We fit the abundances of 14 elements for 48,659 red-giant stars from APOGEE DR17 using a flexible, data-driven K-process model---dubbed KPM. In our fiducial model, with K=2, each abundance in each star is described as the sum of a...

87. Closing the loop: observing Gaia white dwarfs with SDSS V

Nicola Pietro Gentile Fusillo

8/1/23, 2:18 PM

Over 95% of all stars in the Galaxy share the same fate: to become a white dwarf.
These small, slowly cooling stellar remnants not only encode the stellar formation history of the Milky Way, but are also unique tools with application spanning a wide range of disciplines from stellar evolution to the study of exoplanets, from exotic physics in extreme environments to the origin of type Ia...

89. GROUP PHOTO

88. LIGHTNING TALKS

32. MWM 101 (TBD?)

34. TBD

Elena D'Onghia