CRIRES: a high-resolution infrared spectrograph for ESO's VLT

Kaeufl, H. U.; Ballester, P.; Biereichel, P.; Délabre, Bernard; Donaldson, Rob; Dorn, Reinhold J.; Fedrigo, Enrico; Finger, Gert; Fischer, Gerhard W.; Franza, F.; Gojak, D.; Huster, Gotthard; Jung, Yves; Lizon, Jean-Louis; Mehrgan, Leander; Meyer, Manfred; Moorwood, A. F. M.; Pirard, Jean-François; Paufique, J.; Pozna, Eszter; Siebenmorgen, R.; Silber, A.; Stegmeier, Joerg; Wegerer, Stefan

doi:10.1117/12.551480

Cited by 250 publications

(86 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…10) targeted by Fedele et al (2011). Our models, in agreement with the observations, predict that this rovibrational line should be undetectable in both T Tauri and Herbig star disks, owing to the sensitivity limits of the CRIRES spectrograph on the VLT (Kaeufl et al 2004). …”

Section: Near-ir Ro-vibrational Water Linessupporting

confidence: 75%

Mid-IR spectra of pre-main sequence Herbig stars: An explanation for the non-detections of water lines

Antonellini¹,

Kamp²,

Lahuis

et al. 2015

A&A

View full text Add to dashboard Cite

Context. The mid-IR detection rate of water lines in disks around Herbig stars disks is about 5%, while it is around 50% for disks around T Tauri stars. The reason for this is still unclear. Aims. In this study, we want to find an explanation for the different detection rates between low mass and high mass pre-main-sequence stars in the mid-IR regime. Methods. We ran disk models with stellar parameters adjusted to spectral types B9 through M2, using the radiation thermo-chemical disk modelling code ProDiMo. We explored also a small parameter space around a standard disk model, considering dust-to-gas mass ratio, disk gas mass, mixing coefficient for dust settling, flaring index, dust maximum size, and size power law distribution index. We produced convolved spectra at the resolution of Spitzer, IRS, JWST MIRI, and VLT VISIR spectrographs. We applied random noise derived from typical Spitzer spectra for a direct comparison with observations. Results. The strength of the mid-IR water lines correlates directly with the luminosity of the central star. The models show that it is possible to suppress the water emission; however, current observations are not sensitive enough to detect mid-IR lines in disks for most of the explored parameters. The presence of noise in the spectra, combined with the high continuum flux (noise level is proportional to the continuum flux), is the most likely explanation for the non-detections towards Herbig stars. Conclusions. Mid-IR spectra with resolution higher than 20 000 are needed to investigate water in protoplanetary disks. Intrinsic differences in disk structure, such as inner gaps, gas-to-dust ratio, dust size and distribution, and inner disk scale height, between Herbig and T Tauri star disks are able to explain a lower water detection rate in disks around Herbig stars.

show abstract

Section: Near-ir Ro-vibrational Water Linessupporting

confidence: 75%

Mid-IR spectra of pre-main sequence Herbig stars: An explanation for the non-detections of water lines

Antonellini¹,

Kamp²,

Lahuis

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…CO emission at 4.7 μm has been observed with the Cryogenic Infrared Echelle Spectrometer (CRIRES; Kaeufl et al 2004) on the Very Large Telescope (VLT) of the European Southern Observatory (ESO). Most spectra have been taken as part of the ESO Large Program 179.C-0151 (Pontoppidan et al 2011b); some measurements have been added from programs 079.C-0349 and 081.C-0833 as published in van der Plas et al (2015), from program 091.C-0671 as published in Carmona et al (2016), and from program 088.…”

Section: Observations and Samplementioning

confidence: 99%

The Depletion of Water During Dispersal of Planet-Forming Disk Regions

Banzatti

Pontoppidan

Salyk

et al. 2017

ApJ

121

View full text Add to dashboard Cite

We present a new velocity-resolved survey of 2.9 μm spectra of hot H 2 O and OH gas emission from protoplanetary disks, obtained with the Cryogenic Infrared Echelle Spectrometer at the VLT (R ∼ 96,000). With the addition of archival Spitzer-IRS spectra, this is the most comprehensive spectral data set of water vapor emission from disks ever assembled. We provide line fluxes at 2.9-33 μm that probe from the dust sublimation radius at ∼0.05 au out to the region of the water snow line. With a combined data set for 55 disks, we find a new correlation between H 2 O line fluxes and the radius of CO gas emission, as measured in velocity-resolved 4.7 μm spectra (Rco), which probes molecular gaps in inner disks. We find that H 2 O emission disappears from 2.9 μm (hotter water) to 33 μm (colder water) as R co increases and expands out to the snow line radius. These results suggest that the infrared water spectrum is a tracer of inside-out water depletion within the snow line. It also helps clarify an unsolved discrepancy between water observations and models by finding that disks around stars ofgenerally have inner gaps with depleted molecular gas content. We measure radial trends in H 2 O, OH, and CO line fluxes that can be used as benchmarks for models to study the chemical composition and evolution of planet-forming disk regions at 0.05-20 au. We propose that JWST spectroscopy of molecular gas may be used as a probe of inner disk gas depletion, complementary to the larger gaps and holes detected by direct imaging and by ALMA.

show abstract

“…Our study is based on high-resolution, near-infrared spectra obtained with CRIRES, (the CRyogenic high-resolution InfraRed Echelle Spectrograph; Kaeufl et al 2004), mounted on UT1 at ESO's VLT. The data were collected between June 2010 and January 2011 under PID 385.D-0273.…”

Section: Observationsmentioning

confidence: 99%

Exploring the magnetic field complexity in M dwarfs at the boundary to full convection

Shulyak

Reiners

Seemann

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Magnetic fields play a pivotal role in the formation and evolution of low-mass stars, but the dynamo mechanisms generating these fields are poorly understood. Measuring cool star magnetism is a complicated task because of the complexity of cool star spectra and the subtle signatures of magnetic fields. Aims. Based on detailed spectral synthesis, we carry out quantitative measurements of the strength and complexity of surface magnetic fields in the four well-known M dwarfs GJ 388, GJ 729, GJ 285, and GJ 406 that populate the mass regime around the boundary between partially and fully convective stars. Very high-resolution (R = 100 000), high signal-to-noise (up to 400), near-infrared Stokes I spectra were obtained with CRIRES at ESO's Very Large Telescope covering regions of the FeH Wing-Ford transitions at 1 μm and Na i lines at 2.2 μm.Methods. A modified version of the Molecular Zeeman Library (MZL) was used to compute Landé g-factors for FeH lines. We determined the distribution of magnetic fields by magnetic spectral synthesis performed with the Synmast code. We tested two different magnetic geometries to probe the influence of field orientation effects. Results. Our analysis confirms that FeH lines are excellent indicators of surface magnetic fields in low-mass stars of type M, particularly in comparison to profiles of Na i lines that are heavily affected by water lines and that suffer problems with continuum normalization. The field distributions in all four stars are characterized by three distinct groups of field components, and the data are consistent neither with a smooth distribution of different field strengths nor with one average field strength covering the full star. We find evidence of a subtle difference in the field distribution of GJ 285 compared to the other three targets. GJ 285 also has the highest average field of 3.5 kG and the strongest maximum field component of 7-7.5 kG. The maximum local field strengths in our sample seem to be correlated with rotation rate. While the average field strength is saturated, the maximum local field strengths in our sample show no evidence of saturation. Conclusions. We find no difference between the field distributions of partially and fully convective stars. The one star with evidence of field distribution different from the other three is the most active star (i.e. with X-ray luminosity and mean surface magnetic field) rotating relatively fast. A possible explanation is that rotation determines the distribution of surface magnetic fields, and that local field strengths grow with rotation even in stars in which the average field is already saturated.

show abstract

CRIRES: a high-resolution infrared spectrograph for ESO's VLT

Cited by 250 publications

References 1 publication

Mid-IR spectra of pre-main sequence Herbig stars: An explanation for the non-detections of water lines

Mid-IR spectra of pre-main sequence Herbig stars: An explanation for the non-detections of water lines

The Depletion of Water During Dispersal of Planet-Forming Disk Regions

Exploring the magnetic field complexity in M dwarfs at the boundary to full convection

Contact Info

Product

Resources

About