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Title: On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates

Journal Article · · The Astrophysical Journal
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  1. Istituto Nazionale di Astrofisica (INAF), Roma (Italy); Space Science Data Center, Roma (Italy)
  2. Istituto Nazionale di Astrofisica (INAF), Roma (Italy); Universidade Federal do Rio Grande do Sul, Porto Alegre (Brazil); Università di Roma Tor Vergata (Italy)
  3. Istituto Nazionale di Astrofisica (INAF), Roma (Italy); Università di Roma Tor Vergata (Italy)
  4. University of Texas, Austin, TX (United States)
  5. Observatories of the Carnegie Institution for Science, Pasadena, CA (United States)
  6. Leibniz-Institut für Astrophysik Potsdam (Germany)
  7. Liverpool John Moores University (United Kingdom)
  8. Georg-August-University Göttingen (Germany)
  9. Universität Heidelberg (Germany)
  10. Université de Nice Sophia-Antipolis (France)
  11. Dartmouth College, Hanover, NH (United States)
  12. Istituto Nazionale di Astrofisica (INAF), Napoli (Italy)
  13. Istituto Nazionale di Astrofisica (INAF), Roma (Italy)
  14. Università degli Studi di Napoli Parthenope (Italy)
  15. Università di Roma Tor Vergata (Italy)
  16. Iowa State University, Ames, IA (United States)
  17. Cerro Tololo Inter-American Observatory (CTIO), La Serena (Chile)
  18. Instituto de Astrofísica de Canarias (IAC), La Laguna (Spain)
  19. University of Tokyo (Japan)
  20. Florida Atlantic University, Boca Raton, FL (United States)
  21. National Research Council, Victoria (Canada)
  22. European Southern Observatory (ESO), Munchen (Germany)
  23. Instituto Milenio de Astrofísica, Santiago (Chile); Pontificia Universidad Catolica de Chile, Santiago (Chile)

We collected the largest spectroscopic catalog of RR Lyrae (RRLs) including ≈20,000 high-, medium-, and low-resolution spectra for ≈10,000 RRLs. We provide the analytical forms of radial velocity curve (RVC) templates. These were built using 36 RRLs (31 fundamental—split into three period bins—and five first-overtone pulsators) with well-sampled RVCs based on three groups of metallic lines (Fe, Mg, Na) and four Balmer lines (H$$α$$, H$$β$$, H$$γ$$, H$$δ$$). We tackled the long-standing problem of the reference epoch to anchor light-curve and RVC templates. For the V-band, we found that the residuals of the templates anchored to the phase of the mean magnitude along the rising branch are ~35% to ~45% smaller than those anchored to the phase of maximum light. For the RVC, we used two independent reference epochs for metallic and Balmer lines and we verified that the residuals of the RVC templates anchored to the phase of mean RV are from 30% (metallic lines) up to 45% (Balmer lines) smaller than those anchored to the phase of minimum RV. We validated our RVC templates by using both the single-point and the three phase point approaches. We found that barycentric velocities based on our RVC templates are two to three times more accurate than those available in the literature. We applied the current RVC templates to Balmer lines RVs of RRLs in the globular NGC 3201 collected with MUSE at VLT. We found the cluster barycentric RV of $$V$$$γ$$ = 496.89 ± 8.37(error) ± 3.43 (standard deviation) km s-1, which agrees well with literature estimates.

Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
USDOE; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF)
OSTI ID:
1983175
Alternate ID(s):
OSTI ID: 23158868
Journal Information:
The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 919; ISSN 0004-637X
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English

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