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De support team!

I am not certain if this is the right place to post request, but it would be great if the Planck all-sky maps were also selectable in the Aladin Lite view in the ESO science portal.

thanks and best wishes

I am reducing newly taken MUSE data from the beginning of 2024. Yet the associated geometry and astrometry files are from April 2021. Where are the newer reference files? Instead of providing a new MASTER_DARK which rarely changes, run the astrometry and geometry calibration sequence more often (considering Chile experiences numerous earthquakes a year, etc.).

Hello, In the ESO Phase 3 Data Release Description (https://www.eso.org/rm/api/v1/public/releaseDescriptions/163) it is indicated (page 5) that "No corrections for barycentric or heliocentric motion have been applied.", but the information is in the header (HIERARCH.ESO.QC.VRAD.BARYCOR or HELICOR, in km/s).

In order to combine (e.g. average) different UVES spectra is it OK to use the header values for correcting manually barycentric or heliocentric motion before the combination of the spectra ? Is there a suggestion for this kind of operation ?

In any case, it is very nice to have these UVES spectra available. Thanks.

The HARPS pipeline generates separate products for both HARPS fibres (labelled A and B), cross correlating the observed spectra with template stellar spectra for various spectral types.

The primary product is a rebinned, combined 1-D spectrum in FITS binary spectroscopic data format. It is accompanied by a TAR file, containing the products of the original pipeline processing, both FITS and non-FITS.

Their content can be identified from their filenames. The root file name is “HARPS.<date_obs>”, where <date_obs> is the start of the observation in the “restricted ISO8601” format. This root name is appended with:

• “_s1d_<fibre>.fits” for 1-D extracted full spectrum, wavelength calibrated, in the solar system barycentric frame (the primary file of the release is the fibre A s1d file converted to the binary table format);

• “_e2ds_<fiber>.fits” for 2-D extracted spectrum, one row per order;

• “_bis_<sptype>_<fiber>.fits” for bisector from the cross correlation computed with the <sptype> mask;

• “_ccf_<sptype>_<fiber>.fits” for cross correlation function matrix for mask for ;

• “_ccf_<sptype>_<fiber>.tbl” for cross correlation function summary table (ASCII) with extracted radial velocity per each order;

• “_INT_GUIDE.fits” for integrated guiding image from the guide camera, used to confirm the correct centering of the star on the fibre. The image is integrated over the whole length of the scientific exposure.

Where:

• <fiber> is either “A” or “B”; in science observations the A fibre is used for the object, while the B fibre is used for ThAr lamp, dark or sky exposure, depending on the observation setup.

• <sptype> is either one of “G2”, “K5” or “M2”, depending on which spectral mask was used in cross-correlation with the spectrum. The pipeline automatically selects one of the masks based on the object’s spectral type, as recorded in the “HIERARCH ESO DPR TYPE” keyword. The “G2” mask is used if the spectral type is G9 or earlier or no spectral type is recorded, the “K5” mask is used for all Kn spectral types, and the “M2” mask is used for spectral types of M0 or later.

edited message -- I need the CCF file for radial velocity correction?

original message

How can I get the ccv file? 

I need the ccv file for radial velocity correction?

I'm trying to locate the slit from an observation available in the data archive ("XS_SRE2" file). I am trying to compare it with integral field spectroscopy data from another instrument (creating a pseudo-slit). For this, I need to locate the X-Shooter slit in the sky.

- Should I use the keywords "CRVARL2", "CDELT2" as offsets (along the slit) from sky coordinate ("RA", "DEC")? In this case, the Position Angle (PA) should be equal to: PA = - "HIERARCH ESO ADA POSANG" (note the negative sign)?

- The XS_SRE2 file has 99 rows (in the sky offset dimension). It seems that the first 33, and the last 33 ones could be discarded, since they appear to be an effect of the Nod&Shuffle technique. Is that that right? This is the reason why there seems to be a contamination (fake aborption) in some rows in the middle (34 -- 66 rows, mainly the extreme ones 34-37 and 63-66)? Also, if I want to the offset in the sky (along the slit) of the row 35 (e.g.), it would be: OFFSET(35) = "CRVARL2" + 34 * "CDELT2"? 

- There is a way to convert the flux units from counts to physical units (e.g. erg/s/cm2/A)?

Thank you,

VISIONS (programme id 198.C-2009, PI J. Alves)

is a Near-Infrared ESO second cycle VISTA Public Survey which covers all major nearby star-forming regions accessible from the southern hemisphere. This imaging survey is designed to deliver deep high-sensitivity observations of areas with large amounts of extinction. It includes also control fields which sample the predominant stellar populations in largely extinction-free regions and multiple epochs imaging data over large areas surrounding the targeted star-forming regions to enable the computation of proper motions for sources inaccessible to Gaia.

This second data release (DR2) contains all the observations on the star-forming region Corona Australis. In total, 160 tiles covering about 43 deg² have been observed, for a total of 3360 files and 0.87 T, between April 2017 and October 2021. The image quality is excellent throughout the entire survey fields with most data featuring point source FWHMs better than 1 arcsec. Compared to 2MASS, the survey reaches up to 6 mag fainter sensitivity limits.

For each observed field, photometrically and astrometrically calibrated tiles and stacked pawprints, together with a corresponding source table are published and available via the Archive Science Portal or programmatically.

A detailed description of the released data is available in the related documentation.

The APEX telescope has obtained CO(2-1) spectra for a sample of 165 hard-X-Ray-selected AGN galaxies detected in observations by the Burst Alert Telescope (BAT) onboard Swift. These observations, taken under the ESO programme id 198.A-0708, PI M. Koss, allow a statistical comparison of AGN and non-AGN dominated

galaxies in the local Universe, for example from the ALLSMOG APEX survey.

As this programme mainly aimed at observing a statistical sample of
nearby AGN, many of the galaxies observed are well-known galaxies, and these Phase 3 data can provide a valuable total power measurement of the CO(2-1) emission which then can be combined with interferometric observations obtained with ALMA.

Additionally, the BASS (BAT AGN Spectroscopic Survey) sample includes a variety of other ESO data products including hundreds of spectra with VLT/Xshooter, VLT/MUSE, and VLT/FORS2 with more information at the BASS survey website.

This BAT AGN release available via the Science Portal or programatically, makes the combined CO(2-1) spectra publicly available so users can derive further spectroscopic parameters, and compare them with other lines in these objects. The spectra either have a peak S/N>5 or reach depths of 0.5-2 mK rms for non-detections. Further details can be found in the data release paper or in the accompanying release description.

Instructions on how to read or display data in the ESO/SDP tabular data format can be found in the 1D spectrum data format help page.