SVO Filter Profile Service Version 1.0

Rodrigo, C.; Solano, E.; Bayo, A.

doi:10.5479/ads/bib/2012ivoa.rept.1015r

Cited by 237 publications

(182 citation statements)

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“…The theoretical spectra for WDs of spectral type DA with pure hydrogen atmospheres were obtained from Koester (2010), which are mentioned as WD models in the rest of the paper. The spectra were converted to synthetic photometry for the required filters using VOSA (Bayo et al 2008), according to the individual filter profiles (Rodrigo et al 2012(accessed Dec 2018. Extinction of A V = 0.1736 and distance 831±11 pc were used to normalise the SEDs.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

UVIT Open Cluster Study. II. Detection of Extremely Low Mass White Dwarfs and Post–Mass Transfer Binaries in M67

Jadhav

Sindhu

Subramaniam

2019

ApJ

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A detailed study of the ultraviolet (UV) bright stars in the old open star cluster, M67 is presented based on the far-UV observations using the Ultra Violet Imaging Telescope (UVIT) on ASTROSAT. The UV and UV-optical colour-magnitude diagrams (CMDs) along with overlaid isochrones are presented for the member stars, which include blue straggler stars (BSSs), triple systems, white dwarfs (WDs) and spectroscopic binaries (SB). The CMDs suggest the presence of excess UV flux in many members, which could be extrinsic or intrinsic to them. We construct multi-wavelength spectral energy distribution (SED) using photometric data from the UVIT, Gaia DR2, 2MASS and WISE surveys along with optical photometry. We fitted model SEDs to 7 WDs and find 4 of them have mass > 0.5 M and cooling age of less than 200 Myr, thus demanding BSS progenitors. SED fits to 23 stars detect extremely low mass (ELM) WD companions to WOCS2007, WOCS6006 and WOCS2002, and a low mass WD to WOCS3001, which suggest these to be post mass transfer (MT) systems. 12 sources with possible WD companion need further confirmation. 9 sources have X-ray and excess UV flux, possibly arising out of stellar activity. This study demonstrates that UV observations are key to detect and characterise the ELM WDs in non-degenerate systems, which are ideal test beds to explore the formation pathways of these peculiar WDs. The increasing detection of post-MT systems among BSSs and main-sequence stars suggest a strong MT pathway and stellar interactions in M67.

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Section: Spectral Energy Distributionmentioning

confidence: 99%

UVIT Open Cluster Study. II. Detection of Extremely Low Mass White Dwarfs and Post–Mass Transfer Binaries in M67

Jadhav

Sindhu

Subramaniam

2019

ApJ

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“…This research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/) supported from the Spanish MINECO through grant AyA2014-55216. See Rodrigo, Solano & Bayo (2012) for more details on the SVO Filter Profile Service. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/ dpac/consortium).…”

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confidence: 99%

ASASSN-18tb: a most unusual Type Ia supernova observed by TESS and SALT

Vallely

Fausnaugh

Jha

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present photometric and spectroscopic observations of the unusual Type Ia supernova ASASSN-18tb, including a series of SALT spectra obtained over the course of nearly six months and the first observations of a supernova by the Transiting Exoplanet Survey Satellite (TESS). We confirm a previous observation by Kollmeier et al. (2019) showing that ASASSN-18tb is the first relatively normal Type Ia supernova to exhibit clear broad (∼ 1000 km s −1 ) Hα emission in its nebular phase spectra. We find that this event is best explained as a sub-Chandrasekhar mass explosion producing M N i ≈ 0.3 M . Despite the strong Hα signature at late times, we find that the early rise of the supernova shows no evidence for deviations from a single-component power-law and is best fit with a moderately shallow power-law of index 1.69 ± 0.04. We find that the Hα luminosity remains approximately constant after its initial detection at phase +37 d, and that the Hα velocity evolution does not trace that of the Fe III λ4660 emission. These suggest that the Hα emission arises from a circumstellar medium (CSM) rather than swept up material from a non-degenerate companion. However, ASASSN-18tb is strikingly different from other known CSM-interacting Type Ia supernovae in a number of significant ways. Those objects typically show an Hα luminosity two orders of magnitude higher than what is seen in ASASSN-18tb, pushing them away from the empirical light curve relations that define "normal" Type Ia supernovae. Conversely, ASASSN-18tb exhibits a fairly typical light curve and luminosity for an underluminous or transitional SN Ia, with M R ≈ −18.1 mag. Moreover, ASASSN-18tb is the only SN Ia showing Hα from CSM interaction to be discovered in an early-type galaxy.

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“…For each synthetic spectrum, we calculated the absolute magnitude from the flux through each of the SkyMapper u, v, g, and i filters. First, we retrieved the bandpasses of each of the SkyMapper filters (Bessell et al 2011) from the Spanish Virtual Observatory (SVO) Filter Profile Service (Rodrigo et al 2012) 1 . We then closely followed the methodology in Casagrande & Van-denBerg (2014) to generate synthetic magnitudes for each of our synthetic spectra.…”

Section: Generating Synthetic Photometrymentioning

confidence: 99%

Stellar Metallicities from SkyMapper Photometry I: A Study of the Tucana II Ultra-faint Dwarf Galaxy

Chiti¹,

Frebel²,

Jerjen

et al. 2020

ApJ

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We present a study of the ultra-faint Milky Way dwarf satellite galaxy Tucana II using deep photometry from the 1.3 m SkyMapper telescope at Siding Spring Observatory, Australia. The SkyMapper filter-set contains a metallicity-sensitive intermediate-band v filter covering the prominent Ca II K feature at 3933.7Å. When combined with photometry from the SkyMapper u, g, and i filters, we demonstrate that v band photometry can be used to obtain stellar metallicities with a precision of ∼ 0.20 dex when [Fe/H] > −2.5, and ∼ 0.34 dex when [Fe/H] < −2.5. Since the u and v filters bracket the Balmer Jump at 3646Å, we also find that the filter-set can be used to derive surface gravities. We thus derive photometric metallicities and surface gravities for all stars down to a magnitude of g ∼ 20 within ∼75 arcminutes of Tucana II. Photometric metallicity and surface gravity cuts remove nearly all foreground contamination. By incorporating Gaia proper motions, we derive quantitative membership probabilities which recover all known members on the red giant branch of Tucana II. Additionally, we identify multiple likely new members in the center of the system and candidate members several half-light radii from the center of the system. Finally, we present a metallicity distribution function derived from the photometric metallicities of likely Tucana II members. This result demonstrates the utility of wide-field imaging with the SkyMapper filter-set in studying UFDs, and in general, low surface brightness populations of metal-poor stars. Upcoming work will clarify the membership status of several distant stars identified as candidate members of Tucana II.

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SVO Filter Profile Service Version 1.0

Cited by 237 publications

References 0 publications

UVIT Open Cluster Study. II. Detection of Extremely Low Mass White Dwarfs and Post–Mass Transfer Binaries in M67

UVIT Open Cluster Study. II. Detection of Extremely Low Mass White Dwarfs and Post–Mass Transfer Binaries in M67

ASASSN-18tb: a most unusual Type Ia supernova observed by TESS and SALT

Stellar Metallicities from SkyMapper Photometry I: A Study of the Tucana II Ultra-faint Dwarf Galaxy

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