Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Mazeh, T.; Prato, L.; Simon, M.; Goldberg, Elad; Norman, Dara; Zucker, S.

doi:10.1086/324404

Cited by 43 publications

(54 citation statements)

References 26 publications

(38 reference statements)

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“…We analyzed the spectra, following the procedure described in Mazeh et al (2002), with the TODCOR algorithm, which uses a two-dimensional cross-correlation for the analysis of composite spectra (Zucker & Mazeh 1994). Table 3 presents the results for each target; columns (1) and (2) list, respectively, the Julian Date and the orbital phase of the observation.…”

Section: Resultsmentioning

confidence: 99%

“…For example, for two blackbodies of temperatures 5000 and 3000 K, the ratio of the Planck functions at 5000 Å is about 50, whereas at 1.555 lm, the ratio is about 4. Mazeh et al (2002) demonstrate the efficacy of this technique, applied to three main-sequence SB1s. Mazeh et al (1997) used an intermediate approach, detecting mainsequence binaries with mass ratios of 0.57 AE 0.02 and 0.48 AE 0.03 in the R band.…”

Section: Introductionmentioning

confidence: 94%

“…The spectral type appears in column (2), as provided by the Centre de Données astronomiques de Strasbourg (SIMBAD). Column (3) lists the Julian Date of the observation and column (4) the derived radial velocity (Mazeh et al 2002). All but eight of the template stars have radial velocities measured by the Geneva (Duquennoy & Mayor 1991) or CfA groups (Latham 1985).…”

Section: Template Spectramentioning

confidence: 99%

“…SMALLEST MASS RATIO SPECTROSCOPIC BINARIESvelocities relative to , q = (v 1 À )/( Àv 2 ) (Mazeh et al 2002). Values for appear at the top of each section of Table 3, adjacent to the target names.…”

Section: No 2 2002mentioning

confidence: 99%

“…A summary appears in x 6. Previous reports on applications of this technique have appeared in Prato (1998), Steffen et al (2001), and Mazeh et al (2002 Spectra of the target objects were obtained in 2000 June and July and in 2001 January and June; specific dates and target properties appear in Table 1. We used NIRSPEC, the W. M. Keck Observatory's cross-dispersed near-IR cryogenic spectrometer (McLean et al 1998(McLean et al , 2000.…”

Section: Introductionmentioning

confidence: 99%

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The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

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101

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Using high-resolution near-infrared spectroscopy with the Keck Telescope, we have detected the radial velocity signatures of the cool secondary components in four optically identified pre-main-sequence, singlelined spectroscopic binaries. All are weak-lined T Tauri stars with well-defined center-of-mass velocities. The mass ratio for one young binary, NTTS 160905À1859, is M 2 /M 1 = 0.18 AE 0.01, the smallest yet measured dynamically for a pre-main-sequence spectroscopic binary. These new results demonstrate the power of infrared spectroscopy for the dynamical identification of cool secondaries. Visible-light spectroscopy, to date, has not revealed any pre-main-sequence secondary stars with masses <0.5 M , while two of the young systems reported here are in that range. We compare our targets with a compilation of the published young, double-lined spectroscopic binaries and discuss our unique contribution to this sample.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 94%

Section: Template Spectramentioning

confidence: 99%

Section: No 2 2002mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

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101

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Binaries and Multiple Stellar Systems

Horch¹

2013

Planets, Stars and Stellar Systems

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High-resolution infrared spectroscopy as a tool to detect false positives of transit search programs

Guenther

Tal-Or

2010

A&A

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Context. Transit search programs such as CoRoT and Kepler now have the capability of detecting planets as small as the Earth. The detection of these planets however requires the removal of all false positives. Although many false positives can be identified by a detailed analysis of the light-curves (LCs), the detections of others require additional observations. An important source of false positives are faint eclipsing binaries within the point spread function (PSF) of the target star. For example, triple stars are an important source of false positives. Unfortunately, most of the methods previously applied have difficulties in detecting these objects. Aims. We develop a new method that allows us to detect faint eclipsing binaries with a separation smaller than one arcsec from target stars. We thereby focus on binaries that mimic the transits of terrestrial planets. These binaries can be either at the same distance as the target star (triple stars), or at either larger, or smaller distances. Methods. A close inspection of the problem indicates that these systems contain either late-type stars, or stars of high extinction. Thus, in both cases the binaries are brighter in the infrared than in the optical regime. We show how high resolution infrared (hereafter IR) spectroscopy can be used to remove these false positives. Results. For the triple star case, we find that the brightness difference between a primary and an eclipsing secondary is about 9−10 mag in the visual but only about 4.5−5.9 mag in the K-band. In the next step, we demonstrate how the triple star hypothesis can be excluded by taking a high-resolution IR spectrum. Simulations of these systems show that the companions can be detected with a false-alarm probability of ∼2%, if the spectrum has a signal-to-noise ratio (S /N) ≥ 100. We subsequently show that high-resolution IR spectra also allows to detect most of the false positives caused by foreground or background binaries. Conclusions. If high resolution IR spectroscopy is combined with photometric methods, virtually all false positives can be detected without radial velocity (RV) measurements. It is thus possible to confirm transiting terrestrial planets with a modest investment of observing time.

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Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Cited by 43 publications

References 26 publications

The Smallest Mass Ratio Young Star Spectroscopic Binaries

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Binaries and Multiple Stellar Systems

High-resolution infrared spectroscopy as a tool to detect false positives of transit search programs

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