On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates
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 f...
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IOP Publishing
2021-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ac1074 |
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| author | V. F. Braga J. Crestani M. Fabrizio G. Bono C. Sneden G. W. Preston J. Storm S. Kamann M. Latour H. Lala B. Lemasle Z. Prudil G. Altavilla B. Chaboyer M. Dall’Ora I. Ferraro C. K. Gilligan G. Fiorentino G. Iannicola L. Inno S. Kwak M. Marengo S. Marinoni P. M. Marrese C. E. Martínez-Vázquez M. Monelli J. P. Mullen N. Matsunaga J. Neeley P. B. Stetson E. Valenti M. Zoccali |
| author_facet | V. F. Braga J. Crestani M. Fabrizio G. Bono C. Sneden G. W. Preston J. Storm S. Kamann M. Latour H. Lala B. Lemasle Z. Prudil G. Altavilla B. Chaboyer M. Dall’Ora I. Ferraro C. K. Gilligan G. Fiorentino G. Iannicola L. Inno S. Kwak M. Marengo S. Marinoni P. M. Marrese C. E. Martínez-Vázquez M. Monelli J. P. Mullen N. Matsunaga J. Neeley P. B. Stetson E. Valenti M. Zoccali |
| author_sort | V. F. Braga |
| collection | DOAJ |
| description | 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. |
| first_indexed | 2024-03-12T02:01:34Z |
| format | Article |
| id | doaj.art-bddd061a9ae74f6b8a1a2b3d68860a0e |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T02:01:34Z |
| publishDate | 2021-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-bddd061a9ae74f6b8a1a2b3d68860a0e2023-09-07T14:50:16ZengIOP PublishingThe Astrophysical Journal1538-43572021-01-0191928510.3847/1538-4357/ac1074On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve TemplatesV. F. Braga0https://orcid.org/0000-0001-7511-2830J. Crestani1https://orcid.org/0000-0001-8926-3496M. Fabrizio2https://orcid.org/0000-0001-5829-111XG. Bono3https://orcid.org/0000-0002-4896-8841C. Sneden4https://orcid.org/0000-0002-3456-5929G. W. Preston5J. Storm6https://orcid.org/0000-0002-8627-6096S. Kamann7https://orcid.org/0000-0001-6604-0505M. Latour8https://orcid.org/0000-0002-7547-6180H. Lala9B. Lemasle10Z. Prudil11https://orcid.org/0000-0001-5497-5805G. Altavilla12https://orcid.org/0000-0002-9934-1352B. Chaboyer13https://orcid.org/0000-0003-3096-4161M. Dall’Ora14https://orcid.org/0000-0001-8209-0449I. Ferraro15https://orcid.org/0000-0001-8514-7957C. K. Gilligan16https://orcid.org/0000-0003-4510-0964G. Fiorentino17https://orcid.org/0000-0003-0376-6928G. Iannicola18https://orcid.org/0000-0001-9816-5484L. Inno19https://orcid.org/0000-0002-0271-2664S. Kwak20M. Marengo21https://orcid.org/0000-0001-9910-9230S. Marinoni22https://orcid.org/0000-0001-7990-6849P. M. Marrese23https://orcid.org/0000-0002-8162-3810C. E. Martínez-Vázquez24https://orcid.org/0000-0002-9144-7726M. Monelli25https://orcid.org/0000-0001-5292-6380J. P. Mullen26https://orcid.org/0000-0002-1650-2764N. Matsunaga27J. Neeley28https://orcid.org/0000-0002-8894-836XP. B. Stetson29https://orcid.org/0000-0001-6074-6830E. Valenti30https://orcid.org/0000-0002-6092-7145M. Zoccali31https://orcid.org/0000-0002-5829-2267INAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Space Science Data Center, via del Politecnico snc, I-00133 Roma, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Av. Bento Gonçalves 6500, Porto Alegre 91501-970, Brazil; Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, I-00133 Roma, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Space Science Data Center, via del Politecnico snc, I-00133 Roma, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, I-00133 Roma, ItalyDepartment of Astronomy and McDonald Observatory, The University of Texas , Austin, TX 78712, USAThe Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USALeibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482, Potsdam, GermanyAstrophysics Research Institute, Liverpool John Moores University , IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool,L3 5RF, UKInstitute for Astrophysics, Georg-August-University Göttingen , Friedrich-Hund-Platz 1, D-37077 Göttingen, GermanyAstronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, D-69120 Heidelberg, GermanyAstronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, D-69120 Heidelberg, GermanyUniversité de Nice Sophia-antipolis, CNRS, Observatoire de la Côte d’Azur, Laboratoire Lagrange, BP 4229, F-06304 Nice, FranceINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Space Science Data Center, via del Politecnico snc, I-00133 Roma, ItalyDepartment of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USAINAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, ItalyDepartment of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USAINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, ItalyUniversità degli Studi di Napoli Parthenope, Via Amm.F. Acton, 38, I-80133 Napoli, ItalyDipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, I-00133 Roma, ItalyDepartment of Physics and Astronomy, Iowa State University , Ames, IA 50011, USAINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Space Science Data Center, via del Politecnico snc, I-00133 Roma, ItalyINAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; Space Science Data Center, via del Politecnico snc, I-00133 Roma, ItalyCerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, ChileInstituto de Astrofísica de Canarias, Calle Via Lactea s/n, E-38205 La Laguna, Tenerife, SpainDepartment of Physics and Astronomy, Iowa State University , Ames, IA 50011, USADepartment of Astronomy, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanDepartment of Physics, Florida Atlantic University , 777 Glades Rd, Boca Raton, FL 33431 USAHerzberg Astronomy and Astrophysics, National Research Council, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, CanadaEuropean Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei Munchen, GermanyInstituto Milenio de Astrofísica, Santiago, Chile; Pontificia Universidad Catolica de Chile, Instituto de Astrofisica, Av. Vicuña Mackenna 4860, Santiago, ChileWe 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.https://doi.org/10.3847/1538-4357/ac1074RR Lyrae variable starsAtomic spectroscopyRadial velocityGlobular star clusters |
| spellingShingle | V. F. Braga J. Crestani M. Fabrizio G. Bono C. Sneden G. W. Preston J. Storm S. Kamann M. Latour H. Lala B. Lemasle Z. Prudil G. Altavilla B. Chaboyer M. Dall’Ora I. Ferraro C. K. Gilligan G. Fiorentino G. Iannicola L. Inno S. Kwak M. Marengo S. Marinoni P. M. Marrese C. E. Martínez-Vázquez M. Monelli J. P. Mullen N. Matsunaga J. Neeley P. B. Stetson E. Valenti M. Zoccali On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates The Astrophysical Journal RR Lyrae variable stars Atomic spectroscopy Radial velocity Globular star clusters |
| title | On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates |
| title_full | On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates |
| title_fullStr | On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates |
| title_full_unstemmed | On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates |
| title_short | On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates |
| title_sort | on the use of field rr lyrae as galactic probes v optical and radial velocity curve templates |
| topic | RR Lyrae variable stars Atomic spectroscopy Radial velocity Globular star clusters |
| url | https://doi.org/10.3847/1538-4357/ac1074 |
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