Resultados totales (Incluyendo duplicados): 35919
Encontrada(s) 3592 página(s)
Encontrada(s) 3592 página(s)
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365464
Dataset. 2023
X-SHOOTING ULLYSES. PROJECT DESCRIPTION [DATASET]
- Kehrig, C.
Observations of individual massive stars, super-luminous supernovae, gamma-ray bursts, and gravitational wave events involving spectacular black hole mergers indicate that the low-metallicity Universe is fundamentally different from our own Galaxy. Many transient phenomena will remain enigmatic until we achieve a firm understanding of the physics and evolution of massive stars at low metallicity (Z). The Hubble Space Telescope has devoted 500 orbits to observing ~250 massive stars at low Z in the ultraviolet (UV) with the COS and STIS spectrographs under the ULLYSES programme. The complementary X-Shooting ULLYSES (XShootU) project provides an enhanced legacy value with high-quality optical and near-infrared spectra obtained with the wide-wavelength coverage X-shooter spectrograph at ESO's Very Large Telescope. We present an overview of the XShootU project, showing that combining ULLYSES UV and XShootU optical spectra is critical for the uniform determination of stellar parameters such as effective temperature, surface gravity, luminosity, and abundances, as well as wind properties such as mass-loss rates as a function of Z. As uncertainties in stellar and wind parameters percolate into many adjacent areas of astrophysics, the data and modelling of the XShootU project is expected to be a game changer for our physical understanding of massive stars at low Z. To be able to confidently interpret James Webb Space Telescope spectra of the first stellar generations, the individual spectra of low-Z stars need to be understood, which is exactly where XShootU can deliver., In Table B.1 we present optical and NIR (JHK) photometry of the ULLYSES targets, as well as spectroscopic and multiplicity information. Table B.2 provides an extensive literature search for the stellar and wind parameters as they were known prior to the start of ULLYSES., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365464, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A154
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365464
HANDLE: http://hdl.handle.net/10261/365464, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A154
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365464
PMID: http://hdl.handle.net/10261/365464, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A154
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365464
Ver en: http://hdl.handle.net/10261/365464, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A154
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365464
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365465
Dataset. 2023
HN LIB RADIAL VELOCITIES [DATASET]
- Amado, P. J.
- Rodríguez, E.
- Rodríguez- López, C.
- López- González, M. J.
We report the discovery of HN Lib b, a sub-Neptunian mass planet orbiting the nearby (d~6.25pc) M4.0 V star HN Lib detected by our CARMENES radial-velocity (RV) survey. We determined a planetary minimum mass of M_b_sini=5.46+/-0.75M_Earth_ and an orbital period of P_b_=36.116+/-0.029d, using ~5yr of CARMENES data, as well as archival RVs from HARPS and HIRES spanning more than 13yr. The flux received by the planet equals half the instellation on Earth, which places it in the middle of the conservative habitable zone (HZ) of its host star. The RV data show evidence for another planet candidate with M_[c]_sini=9.7+/-1.9M_Earth_ and P_[c]_=113.46+/-0.20d. The long-term stability of the signal and the fact that the best model for our data is a two-planet model with an independent activity component stand as strong arguments for establishing a planetary origin. However, we cannot rule out stellar activity due to its proximity to the rotation period of HN Lib, which we measured using CARMENES activity indicators and photometric data from a ground-based multi-site campaign as well as archival data. The discovery adds HN Lib b to the shortlist of super-Earth planets in the habitable zone of M dwarfs, but HN Lib [c] probably cannot be inhabited because, if confirmed, it would most likely be an icy giant., HN Lib was spectroscopically observed with CARMENES between 27 January 2016 and 31 December 2020, resulting in a total of 94 RV measurements. CARMENES is installed at the 3.5m telescope of the Calar Alto Observatory in Almeria (Spain). It was specifically designed to deliver high-resolution spectra at optical (resolving power R~94600) and near-infrared (R~80400) wavelengths covering the range from 520nm to 1710nm. CARMENES has two different channels, one for the optical (the VIS channel) and one for the near-infrared (the NIR channel) with a dichroic at 960nm. All data were acquired with integration times of 1800s, which is the maximum exposure time employed for precise RV measurements with CARMENES., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365465, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.141G, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A141
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365465
HANDLE: http://hdl.handle.net/10261/365465, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.141G, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A141
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365465
PMID: http://hdl.handle.net/10261/365465, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.141G, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A141
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365465
Ver en: http://hdl.handle.net/10261/365465, https://ui.adsabs.harvard.edu/abs/2023A&A...675A.141G, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A141
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365465
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365466
Dataset. 2023
TIME EVOLUTION OF MRK501 EMISSION DURING 2017-2020 [DATASET]
- Agudo, I.
- Bernardos, M. I.
- Castro-Tirado, A. J.
- Escudero, J.
- López-Coto, R.
- Finke, J.
- Stojanovic, M.
We study the broadband emission of Mrk 501 using multiwavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi's Large Area Telescope (LAT), NuSTAR, Swift, GASP-WEBT, and the Owens Valley Radio Observatory. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wave bands, with the highest occurring at X-rays and very-high-energy (VHE) {gamma}-rays. A significant correlation (>3{sigma}) between X-rays and VHE {gamma}-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between the Swift X-Ray Telescope and Fermi-LAT. We additionally find correlations between high-energy {gamma}-rays and radio, with the radio lagging by more than 100 days, placing the {gamma}-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE {gamma}-rays from mid-2017 to mid-2019 with a stable VHE flux (>0.2TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2yr long low state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED toward the low state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock., This study focuses on the multiwavelength (MWL) data collected from Mrk 501 during the 4yr period spanning from the beginning of the observational period in the year 2017 until the end of the observational period in the year 2020 (MJD 57754 to MJD 59214). The coordinated observations involve a large number of instruments, including FACT, MAGIC, Fermi-LAT, Swift, GLAST-AGILE Support Program (GASP)-Whole Earth Blazar Telescope (WEBT), and OVRO. Additionally, three 10hr long observations with NuSTAR yielded a precise measurement of the falling segment of the low-energy bump, which is expected to be dominated by the highest-energy electrons at the source., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365466, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...37A, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/37
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365466
HANDLE: http://hdl.handle.net/10261/365466, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...37A, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/37
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365466
PMID: http://hdl.handle.net/10261/365466, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...37A, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/37
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365466
Ver en: http://hdl.handle.net/10261/365466, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...37A, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/37
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365466
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365467
Dataset. 2023
EXTENSION OF HOPS OUT TO 500PC (EHOPS). I. AQUILA [DATASET]
- Osorio, Mayra
We present a Spitzer/Herschel focused survey of the Aquila molecular clouds (d~436pc) as part of the eHOPS (extension of the Herschel orion protostar survey, or HOPS, Out to 500 ParSecs) census of nearby protostars. For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1-850{mu}m SEDs assembled from the Two Micron All Sky Survey, Spitzer, Herschel, the Wide-field Infrared Survey Explorer, and James Clerk Maxwell Telescope/SCUBA-2 data. Using a newly developed set of criteria, we classify objects by their SEDs as protostars, pre-main-sequence stars with disks, and galaxies. A total of 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these, 71 (42%) are Class 0 protostars, 54 (31%) are Class I protostars, 43 (25%) are flat-spectrum protostars, and four (2%) are Class II sources. Ten of the Class 0 protostars are young PACS bright red sources similar to those discovered in Orion. We compare the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities, and envelope masses of the protostars. A comparison of the eHOPS-Aquila to the HOPS protostars in Orion finds that the protostellar luminosity functions in the two star-forming regions are statistically indistinguishable, the bolometric temperatures/envelope masses of eHOPS-Aquila protostars are shifted to cooler temperatures/higher masses, and the eHOPS-Aquila protostars do not show the decline in luminosity with evolution found in Orion. We briefly discuss whether these differences are due to biases between the samples, diverging star formation histories, or the influence of environment on protostellar evolution., This paper presents SEDs assembled from photometry and spectra covering a wavelength range of 1-850um. These come from multiple catalogs. The photometry from 1-24um is from the Spitzer Extended Solar Neighborhood Archive (SESNA) catalog compiled by R. Gutermuth et al. (2022, in preparation). The SESNA data products are publicly available through http://bit.ly/sesna2021 We use observations from the Herschel Space Observatory to extract photometry in the 70-500um wavelength region. We obtain the observations from the Herschel Science Archive. We provide the observational details such as observation IDs, observed wavelengths, proposal names, and scan velocities for these observations in Appendix A (Tables 7 and 8). The 850um photometry is from maps made with the Submillimeter Common-User Bolometer Array-2 (SCUBA-2) instrument on the James Clerk Maxwell Telescope (JCMT). We use the 850um flux maps from the JCMT Gould Belt Survey data release repository (Kirk+ 2018ApJS..238....8K ; doi: 10.11570/18.0005). When available, we complement the Spitzer photometry with the spectroscopic measurements from the Infrared Spectrograph (IRS) on Spitzer using the Short-Low (SL; 5.2-14um) and Long-Low (LL; 14-38um) modules, both having a low spectral resolution of about 90. We obtain the IRS observation from the Combined Atlas of Sources with Spitzer IRS Spectra (CASSIS). We also utilize mid-IR photometry from the Wide-field Infrared Survey Explorer (WISE). The WISE photometry is retrieved from the AllWISE catalog (see II/328) in the NASA/IPAC Infrared Science Archive (IRSA). After following the steps from Sections 4.1.2-4.1.6, we find a total of 172 protostars (Table 2), 73 pre-main-sequence (pre-MS) stars with disks (Table 9), 24 reddened pre-MS stars with disks (Table 9), 118 galaxies (Table 10), and 12 candidate protostars (Table 11)., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365467, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...32P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/32
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365467
HANDLE: http://hdl.handle.net/10261/365467, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...32P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/32
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365467
PMID: http://hdl.handle.net/10261/365467, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...32P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/32
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365467
Ver en: http://hdl.handle.net/10261/365467, https://ui.adsabs.harvard.edu/abs/2023ApJS..266...32P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/266/32
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365467
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365468
Dataset. 2023
STELLAR MODELS GRIDS WHITE DWARFS, 0.2 TO 8.0 MSUN [DATASET]
- Claret, A.
One of the most reliable means of studying the stellar interior is through the apsidal motion in double line eclipsing binary systems since these systems present errors in masses, radii, and effective temperatures of only a few per cent. On the other hand, the theoretical values of the apsidal motion to be compared with the observed values depend on the stellar masses of the components and more strongly on their radii (fifth power). The main objective of this work is to make available grids of evolutionary stellar models that, in addition to the traditional parameters (e.g. age, mass, logg, Teff), also contain the necessary parameters for the theoretical study of apsidal motion and tidal evolution. This information is useful for the study of the apsidal motion in eclipsing binaries and their tidal evolution, and can also be used for the same purpose in exoplanetary systems., All models were computed using the MESA package. We consider core overshooting for models with masses >=1.2M_{sun}_. For the amount of core overshooting adopted a recent relationship for mass times core overshooting. We adopted for the mixing-length parameter {alpha}_MLT_ the value 1.84 (the solar-calibrated value). Mass loss was taken into account in two evolutionary phases. The models were followed from the pre-main sequence phase to the white dwarf (WD) stage. The evolutionary models containing age, luminosity, logg, and Teff, as well as the first three harmonics of the internal stellar structure (k_2_, k_3_, and k_4_), the radius of gyration {beta} y, and the dimensionless variable {alpha}, related to gravitational potential energy, are presented in 69 tables covering three chemical compositions: [Fe/H] = -0.50, 0.00, and 0.50. Additional models with different input physics are available., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365468, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..67C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A67
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365468
HANDLE: http://hdl.handle.net/10261/365468, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..67C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A67
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365468
PMID: http://hdl.handle.net/10261/365468, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..67C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A67
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365468
Ver en: http://hdl.handle.net/10261/365468, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..67C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A67
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365468
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365469
Dataset. 2023
POWER-2 LIMB-DARKENING COEFFICIENTS [DATASET]
- Claret, A.
The phenomenon of limb-darkening is relevant to many topics in astrophysics, including the analysis of light curves of eclipsing binaries, optical interferometry, measurement of stellar diameters, line profiles of rotating stars, gravitational microlensing, and transits of extrasolar planets. Multiple parametric limb-darkening laws have been presented, and there are many available sources of theoretical limb-darkening coefficients (LDCs) calculated using stellar model atmospheres. The power-2 limb-darkening law allows a very good representation of theoretically predicted intensity profiles, but few LDCs are available for this law from spherically symmetric model atmospheres. We therefore present such coefficients in this work. We computed LDCs for the space missions Gaia, Kepler, TESS, and CHEOPS and for the passbands uvby, UBVRIJHK, and SDSS ugriz, using the PHOENIX-COND spherical models. We adopted two methods to characterise the truncation point, which sets the limb of the star: the first (M1) uses the point where the derivative dI(r)/dr is at its maximum --- where I(r) is the specific intensity as a function of the normalised radius r --- corresponding to {mu}_cri_, and the second (M2) uses the midpoint between the point {mu}_cri_ and the point located at {mu}_cri-1_. The LDCs were computed adopting the Levenberg-Marquardt least-squares minimisation method, with a resolution of 900 equally spaced {mu} points, and covering 823 model atmospheres for a solar metallicity, effective temperatures of 2300 to 12000K, logg values from 0.0 to 6.0, and microturbulent velocities of 2km/s. As our previous calculations of LDCs using spherical models included only 100{mu} points, we also updated the calculations for the four-parameter law for the passbands listed above, and compared them with those from the power-2 law. Comparisons between the quality of the fits provided by the power-2 and four-parameter laws show that the latter presents a lower merit function, chi^2^, than the former for both cases (M1 and M2). This is important when choosing the best approach for a particular science goal., We computed LDCs for the power-2 law using specific intensities from spherical model atmospheres, as such results were only previously available for a small range of stellar parameters. To this end, we used the phoenix-cond models for Te values from 2300K to 12000K, log g values from 0.0 to 6.0, solar metallicity, V_{xi}_=2.0km/s, and with 900 {mu} points. We also computed LDCs for the four-parameter law, which supersede our previous calculations based on only 100 {mu} points. For both laws, we computed coefficients for the uvby, UBVRIJHK; and SDSS ugriz passbands, and for the Gaia, Kepler, TESS, and CHEOPS photometric systems., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365469, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..63C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A63
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365469
HANDLE: http://hdl.handle.net/10261/365469, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..63C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A63
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365469
PMID: http://hdl.handle.net/10261/365469, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..63C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A63
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365469
Ver en: http://hdl.handle.net/10261/365469, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..63C, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A63
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365469
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365470
Dataset. 2023
LINE-BY-LINE SENSITIVITY TO ACTIVITY IN M DWARF [DATASET]
- Lafarga, M.
- Ribas, I.
- Amado, P. J.
- Caballero, J. A.
- Schöfer, P.
Radial velocities (RVs) measured from high-resolution stellar spectra are routinely used to detect and characterise orbiting exoplanet companions. The different lines present in stellar spectra are created by several species, which are non-uniformly affected by stellar variability features such as spots or faculae. Stellar variability distorts the shape of the spectral absorption lines from which precise RVs are measured, posing one of the main problems in the study of exoplanets. In this work we aim to study how the spectral lines present in M dwarfs are independently impacted by stellar activity. We use CARMENES optical spectra of six active early- and mid-type M dwarfs to compute line-by-line RVs and study their correlation with several well-studied proxies of stellar activity. We are able to classify spectral lines based on their sensitivity to activity in five M dwarfs displaying high levels of stellar activity. We further use this line classification to compute RVs with activity-sensitive lines and less sensitive lines, enhancing or mitigating stellar activity effects in the RV time series. For specific sets of the least activity-sensitive lines, the RV scatter decreases by ~2 to 5 times the initial one, depending on the star. Finally, we compare these lines in the different stars analysed, finding the sensitivity to activity to vary from star to star. Despite the high density of lines and blends present in M dwarf stellar spectra, we find that a line-by-line approach is able to deliver precise RVs. Line-by-line RVs are also sensitive to stellar activity effects, and allow for an accurate selection of activity- insensitive lines to mitigate activity effects in RV. However, we find stellar activity effects to vary in the same insensitive lines from star to star., Tables containing information about the sensitivity to activity of the different lines, one table for each of the six stars studied in this work. Each table includes the central wavelength of the line as measured in the spectral template used, the scatter of the line RV, and the Pearson's correlation coefficient R obtained for the correlation between the line RV and the three activity indicators considered (i.e. three different R values, one per indicator). We note that even though we use the term line, these 'lines' correspond to minima in the spectrum and are the result of blends of true atomic lines or features in molecular bands., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365470, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..61L, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A61
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365470
HANDLE: http://hdl.handle.net/10261/365470, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..61L, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A61
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365470
PMID: http://hdl.handle.net/10261/365470, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..61L, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A61
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365470
Ver en: http://hdl.handle.net/10261/365470, https://ui.adsabs.harvard.edu/abs/2023A&A...674A..61L, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A61
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365470
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365471
Dataset. 2023
SN 2020EYJ OPTICAL PHOTOMETRY [DATASET]
- Moldón, Javier
- Pérez-Torres, Miguel
Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star, but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds or binary interaction before explosion, and the supernova ejecta crashing into this nearby circumstellar material should result in radio synchrotron emission. However, despite extensive efforts, no type Ia supernova (SN Ia) has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate white dwarf star. Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich circumstellar material, as demonstrated by its spectral features, infrared emission and, for the first time in a SN Ia to our knowledge, a radio counterpart. On the basis of our modelling, we conclude that the circumstellar material probably originates from a single-degenerate binary system in which a white dwarf accretes material from a helium donor star, an often proposed formation channel for SNe Ia. We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems., SN 2020eyj was first detected on 7 March 2020 UT (modified Julian date (MJD) = 58915.12, at RA=11:11:47.19, DE=29:23:06.5 (J2000). The SN was classified as a SN Ia based on a low-resolution spectrum obtained on 2 April 2020, 25 days after the first detection. We present optical photometry of SN 2020eyj in table 1., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365471, https://ui.adsabs.harvard.edu/abs/2023Natur.617..477K, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/Nat/617.477
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365471
HANDLE: http://hdl.handle.net/10261/365471, https://ui.adsabs.harvard.edu/abs/2023Natur.617..477K, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/Nat/617.477
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365471
PMID: http://hdl.handle.net/10261/365471, https://ui.adsabs.harvard.edu/abs/2023Natur.617..477K, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/Nat/617.477
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365471
Ver en: http://hdl.handle.net/10261/365471, https://ui.adsabs.harvard.edu/abs/2023Natur.617..477K, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/Nat/617.477
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365471
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365472
Dataset. 2023
CARMENES M DWARF TEMPLATE LIBRARY [DATASET]
- Ribas, I.
- Béjar, V. J. S.
- Montes, D.
- Pedraz, S.
Light from celestial objects interacts with the molecules of the Earth's atmosphere, resulting in the production of telluric absorption lines in ground-based spectral data. Correcting for these lines, which strongly affect red and infrared wavelengths, is often needed in a wide variety of scientific applications. Here we present the template division telluric modeling (TDTM) technique, a method to accurately remove telluric absorption lines in stars that exhibit numerous intrinsic features. Based on the Earth's barycentric motion through the year, our approach is suited to disentangle telluric and stellar spectral components. By fitting a synthetic transmission model, telluric-free spectra are derived. We demonstrate the performance of the TDTM technique in correcting telluric contamination using a high-resolution optical spectral time series of the feature-rich M3.0 dwarf star Wolf 294 obtained with the CARMENES spectrograph. We apply the TDTM approach to the CARMENES survey sample, which consists of 382 targets encompassing 22357 optical and 20314 near-infrared spectra, to correct for telluric absorption. The corrected spectra are co-added to construct template spectra for each of our targets. This library of telluric-free, high signal-to-noise ratio (S/N), high-resolution (R>80000) templates comprises the most comprehensive collection of spectral M dwarf data available to date, both in terms of quantity and quality, and is available at the project's website., In Table C.1, we provide the list of stars included in the spectral template library, which features telluric-free, high S/N optical (VIS) and near-infrared (NIR) CARMENES spectra. The individual observations of each star have been corrected for telluric absorption lines using the TDTM technique. Subsequently, the individual spectra have been coadded to produce a high S/N template spectrum for each star. Details in Table C.1 include the the star identifier, coordinates, spectral type, J magnitude, the number of coadded spectra for each VIS and NIR template, and the S/N of each VIS and NIR template. The template spectra are accessible through the CARMENES GTO Data Archive (http://carmenes.cab.inta-csic.es)., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365472, https://ui.adsabs.harvard.edu/abs/2023A&A...680A..73N, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A73
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365472
HANDLE: http://hdl.handle.net/10261/365472, https://ui.adsabs.harvard.edu/abs/2023A&A...680A..73N, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A73
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365472
PMID: http://hdl.handle.net/10261/365472, https://ui.adsabs.harvard.edu/abs/2023A&A...680A..73N, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A73
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365472
Ver en: http://hdl.handle.net/10261/365472, https://ui.adsabs.harvard.edu/abs/2023A&A...680A..73N, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A73
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365472
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365473
Dataset. 2023
HII-CHI-MISTRY-UV FOR AGN. ABUNDANCES [DATASET]
- Pérez-Montero, E.
- Pérez-Díaz, B.
- Vílchez, J. M.
- García-Benito, R.
We present an adapted version of the code HII-CHI-mistry-UV (Perez-Montero & Amorin, 2017MNRAS.467.1287P) to derive chemical abundances from emission lines in the ultraviolet, for use in narrow line regions (NLR) of Active Galactic Nuclei (AGN). We evaluate different ultraviolet emission line ratios and how different assumptions about the models, including the presence of dust grains, the shape of the incident spectral energy distribution, or the thickness of the gas envelope around the central source, may affect the final estimates as a function of the set of emission lines used. We compare our results with other published recipes for deriving abundances using the same emission lines and show that deriving the carbon-to-oxygen abundance ratio using CIII] {lambda}1909{AA} and OIII] {lambda}1665{AA} emission lines is a robust indicator of the metal content in AGN that is nearly independent of model assumptions, similar to the case of star-forming regions. Moreover, we show that a prior determination of C/O allows for a much more precise determination of the total oxygen abundance using carbon UV lines, as op- posed to assuming an arbitrary relationship between O/H and C/O, which can lead to non-negligible discrepancies., Table 2: List of UV fluxes for the sample of AGN and references. Table 3: Chemical abundances estimated from HCm-UV, using the grid of AGN models for alpha(OX)=-1.2 and the stopping criteria of 98% of free electrons. Dust-free or grain-included models are selected based on their C3C4 value., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No
Proyecto: //
DOI: http://hdl.handle.net/10261/365473, https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.1556P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/521/1556
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365473
HANDLE: http://hdl.handle.net/10261/365473, https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.1556P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/521/1556
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365473
PMID: http://hdl.handle.net/10261/365473, https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.1556P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/521/1556
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365473
Ver en: http://hdl.handle.net/10261/365473, https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.1556P, https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/521/1556
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/365473
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