Quick Look Reduced Data

UVES SV Data Products

The data being releasedconsist of the raw and calibration dataalong with fits files of reduced spectra obtained following procedureswhich are fully described for each set of spectra. It is emphasizedthat extraction and reduction of such spectra followed generic prescriptions. Therefore, the reduced spectra released here are intended uniquely to allowusers a quick-look evaluation of the science quality of the data, thushelping the planning for their most effective scientific exploitation.Of course, users who intend to make useof the data are expected to extract and reduce the spectra again, optimizingthe procedures for their own specific scientific goals.

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A Spectroscopic Surveyof Intermediate Redshift QSOs

The spectra given below were obtained  usingthe UVES MIDAS context performing the following steps:
  • bias substraction (object and flat-field))
  • interorder background substraction (object and flat-field)
  • optimal extraction of the object (above thesky, rejecting cosmics)
  • division by a flat-field frame extracted with thesame weigthed-profile as the object
  • wavelength calibration and rebining to 0.05A
  • merging of all overlaping orders
  • heliocentric radial velocity correction
  • coaddition of all extracted spectra
The first order of the blaze function is corrected by the flat-fielding, but  no further attempt has been made to correctfor higher orders. No attempt has been made to get rid of any residualcosmic rays. The spectra are not normalised, nor corrected for atmosphericextinction.
It is noted that the wavelength are given in air (not in vacuum)

Q1101-264 click on the link to request the dataset
QSO_Q1101_B346_b.fits
QSO_Q1101_B437_b.fits
QSO_Q1101_R580_l.fits
QSO_Q1101_R580_u.fits
QSO_Q1101_R860_l.fits
QSO_Q1101_R860_u.fits

HE 1122-1648click on the link to request the dataset
QSO_HE1122_B346_b.fits
QSO_HE1122_B437_b.fits
QSO_HE1122_R580_l.fits
QSO_HE1122_R580_u.fits
QSO_HE1122_R860_l.fits
QSO_HE1122_R860_u.fits

HE 1347-2457click on the link to request the dataset
QSO_HE1347_B437_b.fits
QSO_HE1347_R860_l.fits
QSO_HE1347_R860_u.fits

It is emphasized that extraction and reductionof such spectra followed generic prescriptions.  Therefore, thereduced spectra released here are intended uniquely to allow users a quick-lookevaluation of the science quality of the data, thus helping the planningfor their most effective scientific exploitation. Ofcourse, users who intend to make use of the data are expected to extractand reduce the spectra again, optimizing the procedures for their own specificscientific goals.

Each file is identified by thename of the object plus a setting identifier:
B346_b : dichroic#1 blue armcentered at 346nm
B437_b : dichroic#2 blue armcentered at 437nm
R580_l : dichroic#1 red armcentered at 580nm, EEV (lower) detector
R580_u : dichroic#1 red armcentered at 580nm, MIT (upper) detector
R860_l : dichroic#2 red armcentered at 860nm, EEV (lower) detector
R860_u : dichroic#2 red armcentered at 860nm, MIT (upper) detector


Abundance Ratiosof Extremely Metal Poor stars

The spectra given below were obtained  usingthe UVES MIDAS context performing the following steps:
  • bias substraction (object and flat-field))
  • interorder background substraction (object and flat-field)
  • optimal extraction of the object (above thesky, rejecting cosmics)
  • division by a flat-field frame extracted with thesame weigthed-profile as the object
  • wavelength calibration and rebining to a constantstep
  • merging of all overlaping orders
  • barycentric radial velocity correction
  • coaddition of all extracted spectra
The first order of the blaze function is corrected by the flat-fielding, but  no further attempt has been made to correctfor higher orders. No attempt has been made to get rid of any residualcosmic rays. The spectra are not normalised.

HE 1353-2735(IdentificationChristlieb 2000)click on the link to request the dataset
EMP_HE1353_B470_b.fits
EMP_HE1353_R785_l.fits
EMP_HE1353_R785_u.fits

HE 1303-2708(IdentificationChristlieb 2000)click on the link to request the dataset
EMP_HE1303_B470_b.fits
EMP_HE1303_R785_l.fits
EMP_HE1303_R785_u.fits

In the case of G64-12, however,due to the very high S/N of each of the spectra, the extraction methodwas not optimal but a straight average in an extraction slitof 15 pixels. This method gives a better final S/N, but does not allowto reject cosmic rays during the extraction. All the other steps of reductionare the same as stated above.
G 64-12click on the link to request the dataset
EMP_G64-12_B346_b.fits
EMP_G64-12_R580_l.fits
EMP_G64-12_R580_u.fits
EMP_G64-12_R860_l.fits
EMP_G64-12_R860_u.fits

It is emphasized that extraction and reductionof such spectra followed generic prescriptions.  Therefore, thereduced spectra released here are intended uniquely to allow users a quick-lookevaluation of the science quality of the data, thus helping the planningfor their most effective scientific exploitation. Ofcourse, users who intend to make use of the data are expected to extractand reduce the spectra again, optimizing the procedures for their own specificscientific goals.

Each file is identified by thename of the object plus a setting identifier:
B346_b : dichroic#1 blue armcentered at 346nm
B437_b : dichroic#2 blue armcentered at 437nm
R580_l : dichroic#1 red armcentered at 580nm, EEV (lower) detector
R580_u : dichroic#1 red armcentered at 580nm, MIT (upper) detector
R860_l : dichroic#2 red armcentered at 860nm, EEV (lower) detector
R860_u : dichroic#2 red armcentered at 860nm, MIT (upper) detector


 Chemical Abundancesin LMC Clusters in a Wide Age Range

The spectra given below were obtained  usingthe UVES MIDAS context performing the following steps:
  • bias substraction (object and flat-field))
  • interorder background substraction (object and flat-field)
  • optimal extraction of the object (above thesky, rejecting cosmics)
  • division by a flat-field frame extracted with thesame weigthed-profile as the object
  • wavelength calibration and rebining to a constantstep
  • merging of all overlaping orders
  • barycentric radial velocity correction
  • coaddition of all extracted spectra
The first order of the blaze function is corrected by the flat-fielding, but  no further attempt has been made to correctfor higher orders. No attempt has been made to get rid of any residualcosmic rays. The spectra are not normalised.

NGC 1866(Identification Brocato et al. 1989)click on the link to request the dataset
LMC_N1866_1653_R580_l.fits
LMC_N1866_1653_R580_u.fits
LMC_N1866_444_R580_l.fits
LMC_N1866_444_R580_u.fits
LMC_N1866_867_R580_l.fits
LMC_N1866_867_R580_u.fits

NGC 1978(Identification Loyd & Evans 1980)click on the link to request the dataset
LMC_N1978_LE8_R580_l.fits
LMC_N1978_LE8_R580_u.fits
LMC_N1978_LE9_B437_b.fits
LMC_N1978_LE9_R860_l.fits
LMC_N1978_LE9_R860_u.fits
LMC_N1978_LE9_R580_l.fits
LMC_N1978_LE9_R580_u.fits

ESO 121 (Identification Mateo 1986)click on the link to request the dataset
LMC_E121_M167_R580_l.fits
LMC_E121_M167_R580_u.fits
LMC_E121_M313_R580_l.fits
LMC_E121_M313_R580_u.fits

NGC2210 (IdentificationBrocato et al. 1996)click on the link to request the dataset
LMC_N2210_B110_R580_l.fits
LMC_N2210_B110_R580_u.fits
LMC_N2210_B4364_R580_l.fits
LMC_N2210_B4364_R580_u.fits
LMC_N2210_B4793_R580_l.fits
LMC_N2210_B4793_R580_u.fits

It is emphasized that extraction and reductionof such spectra followed generic prescriptions.  Therefore, thereduced spectra released here are intended uniquely to allow users a quick-lookevaluation of the science quality of the data, thus helping the planningfor their most effective scientific exploitation. Ofcourse, users who intend to make use of the data are expected to extractand reduce the spectra again, optimizing the procedures for their own specificscientific goals.

Each file is identified by thecluster and the object name, plus a setting identifier:
R580_l : Red arm centered at580nm, EEV (lower) detector
R580_u : Red arm centered at580nm, MIT (upper) detector
B437_b : dichroic#2 blue armcentered at 437nm
R860_l : dichroic#2 red armcentered at 860nm, EEV (lower) detector
R860_u : dichroic#2 red armcentered at 860nm, MIT (upper) detector


Supernovae 1987a

 
SN87a

data are currently being verified and prepared for release

It is emphasized that extraction and reductionof such spectra followed generic prescriptions.  Therefore, thereduced spectra released here are intended uniquely to allow users a quick-lookevaluation of the science quality of the data, thus helping the planningfor their most effective scientific exploitation. Ofcourse, users who intend to make use of the data are expected to extractand reduce the spectra again, optimizing the p