The Tycho-2 Spectral Type Catalog

Wright, Candace Oaxaca; Egan, M. P.; Kraemer, K. E.; Price, S. D.

doi:10.1086/345511

Cited by 176 publications

(150 citation statements)

References 7 publications

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“…3.2.2) are typical of a star with B0.5 Ib-a instead of B1 III (Wright et al 2003) or B1 Ib (Garrison et al 1977). There has been a web search on the information presented about the star HD 112364 but it is not presented anywhere as a multiple system.…”

Section: Spectral Classificationmentioning

confidence: 99%

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Corti

Orellana

2013

A&A

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Context. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet.Results. With this investigation we found 52 members of Cen OB1 (l = 303.• 7, b = 0.• 4) and four members of NGC 4755 (l = 303.• 2, b = 2.• 5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ∼−20 km s −1 , μ α cos δ = −4.78 ± 0.10 mas yr −1 , μ δ = −0.93 ± 0.10 mas yr −1 , and ∼20 × 10 6 years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, −18 ± 2 km s −1 , μ α cos δ = −4.14 ± 0.19 mas yr −1 , μ δ = −1.09 ± 0.12 mas yr −1 , and ∼15 × 10 6 years old. The pulsars PSR J1253−5820 and PSR J1254−6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process.

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Section: Spectral Classificationmentioning

confidence: 99%

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Corti

Orellana

2013

A&A

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“…then normalised by a black body profile at the T eff listed in the Tycho-2 Spectral Type Catalog (Wright et al 2003), taking the more relevant absorption spectral features of the stars into account. As discussed in Bedregal et al (2009), in most cases the only spectral features in absorption are the Brackett series so we modelled them using a Lorentzian profile.…”

Section: Data Reductionmentioning

confidence: 99%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(L IR /L ) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs) and with average linear resolutions of ∼0.2 kpc and ∼0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ∼33% of the LIRGs and ∼71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H 2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ∼71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M yr −1 kpc −2 over large areas (4−9 kpc 2 ) with peaks of about 2−2.5 M yr −1 kpc −2 in the smaller regions (0.16 kpc 2 ) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ∼0.4 M yr −1 kpc −2 in somewhat larger areas (100−200 kpc 2 ) and for the Paα peak (∼2 M yr −1 kpc −2 in 4 kpc 2 ). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

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“…977 objects are selected from the Tycho-2 spectral type catalog (Wright et al 2003) while 758 objects are from the Hipparcos catalog (Perryman et al 1997). We select B8V-M9V stars based on the Tycho-2 spectral type catalog (Wright et al 2003), which contains the largest number of stars with information on the luminosity class. The Tycho-2 spectral type catalog is made by combining other original catalogs.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Stars located in the main-sequence locus (M V < 6.0 × (B − V ) − 2.0) are added to our sample. A total 64,209 main-sequence candidates are listed and cross-identified with the AKARI mid-IR PSC sources using a search radius of 3 , because the astrometric accuracy for the Hipparcos catalog, Tycho-2 spectral catalog, and the AKARI mid-IR PSC are ∼0.7 milli-arcsecond, ∼0.5 , and 2 , respectively (Perryman et al 1997;Wright et al 2003;Ishihara et al 2010).…”

Section: Sample Selectionmentioning

confidence: 99%

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Faint warm debris disks around nearby bright stars explored by AKARI and IRSF

Ishihara

Takeuchi

Kobayashi

et al. 2017

A&A

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Context. Debris disks are important observational clues for understanding planetary-system formation process. In particular, faint warm debris disks may be related to late planet formation near 1 au. A systematic search of faint warm debris disks is necessary to reveal terrestrial planet formation. Aims. Faint warm debris disks show excess emission that peaks at mid-IR wavelengths. Thus we explore debris disks using the AKARI mid-IR all-sky point source catalog (PSC), a product of the second generation unbiased IR all-sky survey. Methods. We investigate IR excess emission for 678 isolated main-sequence stars for which there are 18 µm detections in the AKARI mid-IR all-sky catalog by comparing their fluxes with the predicted fluxes of the photospheres based on optical to near-IR fluxes and model spectra. The near-IR fluxes are first taken from the 2MASS PSC. However, 286 stars with Ks<4.5 in our sample have large flux errors in the 2MASS photometry due to saturation. Thus we have measured accurate J, H, and Ks band fluxes, applying neutral density (ND) filters for Simultaneous InfraRed Imager for Unbiased Survey (SIRIUS) on IRSF, the φ1.4 m near-IR telescope in South Africa, and improved the flux accuracy from 14% to 1.8% on average. Results. We identified 53 debris-disk candidates including eight new detections from our sample of 678 main-sequence stars. The detection rate of debris disks for this work is ∼8%, which is comparable with those in previous works by Spitzer and Herschel. Conclusions. The importance of this study is the detection of faint warm debris disks around nearby field stars. At least nine objects have a large amount of dust for their ages, which cannot be explained by the conventional steady-state collisional cascade model.

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The Tycho-2 Spectral Type Catalog

Cited by 176 publications

References 7 publications

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

Faint warm debris disks around nearby bright stars explored by AKARI and IRSF

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