Measurement of T Tauri Binaries Using the Hubble Space Telescope Fine Guidance Sensors

Simon, M.; Holfeltz, S. T.; Taff, L. G.

doi:10.1086/177836

Cited by 43 publications

(65 citation statements)

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“…Ghez et al (1995), Simon, Holfeltz, & Taff (1996), and Steffen et al (2001) take advantage of near-infrared (near-IR) speckle interferometry and the fine guidance sensors available on the HST to map the orbits of young binary systems. Using optical wavelength ($5000 Å ) spectroscopy, Mathieu, Walter, & Myers (1989) and identified 12 young, low-mass, double-lined spectroscopic binaries (SB2s) and 13 singlelined systems (SB1s).…”

Section: Introductionmentioning

confidence: 99%

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: Introductionmentioning

confidence: 99%

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

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101

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“…While the red wing may be caused by scattering, the blue wing may be caused by the combination of the spectra of HV Tau A and B. The binary is close enough (∼0.07 ) to be considered as a point source in our observation, but the objects have similar brightnesses and different colors (Simon et al 1998). We tentatively fitted the absorption peak with the laboratory data to derive the water ice column density.…”

Section: H 2 O Icementioning

confidence: 98%

AKARI observations of ice absorption bands towards edge-on young stellar objects

Aikawa

Kamuro

Sakon

et al. 2012

A&A

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Context. Circumstellar disks and envelopes of low-mass young stellar objects (YSOs) contain significant amounts of ice. Such icy material will evolve to become volatile components of planetary systems, such as comets in our solar system. Aims. To investigate the composition and evolution of circumstellar ice around low-mass young stellar objects (YSOs), we observed ice absorption bands in the near infrared (NIR) towards eight YSOs ranging from class 0 to class II, among which seven are associated with edge-on disks. Methods. We performed slit-less spectroscopic observations using the grism mode of the InfraRed Camera (IRC) on board AKARI, which enables us to obtain full NIR spectra from 2.5 μm to 5 μm, including the CO 2 band and the blue wing of the H 2 O band, which are inaccessible from the ground. We developed procedures to carefully process the spectra of targets with nebulosity. The spectra were fitted with polynomial baselines to derive the absorption spectra. The molecular absorption bands were then fitted with the laboratory database of ice absorption bands, considering the instrumental line profile and the spectral resolution of the grism dispersion element. Results. Towards the class 0-I sources (L1527, IRC-L1041-2, and IRAS 04302), absorption bands of H 2 O, CO 2 , CO, and XCN are clearly detected. Column density ratios of CO 2 ice and CO ice relative to H 2 O ice are 21−28% and 13−46%, respectively. If XCN is OCN − , its column density is as high as 2−6% relative to H 2 O ice. The HDO ice feature at 4.1 μm is tentatively detected towards the class 0-I sources and HV Tau. Non-detections of the CH-stretching mode features around 3.5 μm provide upper limits to the CH 3 OH abundance of 26% (L1527) and 42% (IRAS 04302) relative to H 2 O. We tentatively detect OCS ice absorption towards IRC-L1041-2. Towards class 0-I sources, the detected features should mostly originate in the cold envelope, while CO gas and OCN − could originate in the region close to the protostar, where there are warm temperatures and UV radiation. We detect H 2 O ice band towards ASR41 and 2MASSJ 1628137-243139, which are edge-on class II disks. We also detect H 2 O ice and CO 2 ice towards HV Tau, HK Tau, and UY Aur, and tentatively detect CO gas features towards HK Tau and UY Aur.

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“…Figure 1 shows these steps in processing applied to ZZ Tau as observed along the x-axis of the FGS on 2002 December 6. Balega et al 2002), ZZ Tau (Simon et al 1996), and Elias 12 (Ghez et al 1995;Simon et al 1996;White & Ghez 2001). Column (2) specifies the photometric band for the primary and secondary magnitudes listed in columns (3) and (4).…”

Section: Fine Guidance Sensor Observationsmentioning

confidence: 99%

“…Most of the measurements we report here were taken with the Fine Guidance Sensors on the Hubble Space Telescope (HST) and are a continuation of the program described in Simon, Holfeltz, & Taff (1996). The close pair in Elias 12 was also observed with adaptive optics on the Keck II telescope.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Masses of Young Stars in Multiple Systems

et al. 2003

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We present recent measurements of the orbital motion in the young binaries DF Tau and ZZ Tau and the hierarchical triple Elias 12 that were obtained with the Fine Guidance Sensors on the Hubble Space Telescope and at the Keck Observatory using adaptive optics. Combining these observations with previous measurements from the literature, we compute preliminary orbital parameters for DF Tau and ZZ Tau. We find that the orbital elements cannot yet be determined precisely because the orbital coverage spans only $90 in position angle. Nonetheless, the range of possible values for the period and semimajor axis already defines a useful estimate for the total mass in DF Tau

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Measurement of T Tauri Binaries Using the Hubble Space Telescope Fine Guidance Sensors

Cited by 43 publications

References 0 publications

The Smallest Mass Ratio Young Star Spectroscopic Binaries

The Smallest Mass Ratio Young Star Spectroscopic Binaries

AKARI observations of ice absorption bands towards edge-on young stellar objects

Dynamical Masses of Young Stars in Multiple Systems

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