X-shooter

Importing data from ESO Archive:

a) go to http://archive.eso.org/eso/eso_archive_main.html

b) mark whatever you need, type in date and instrument or type in the ID number of you program

c) press search, check if this is what you want, and mark the data you want to have

d) press instant download

e) save in the download script downloadRequest5157script.sh in the folder you wish your data were

f) change the permission of the script chmod 777 downloadRequest5157script.sh

g) run it: ./downloadRequest5157script.sh

h) check if aqusition images agree with the object

Using ESO PIPELINE

1. Open the GASGANO pipline interface by typing in a terminal gasgano

2. Import data frames (make sure alll imported data are unzipped, otherwise Gasgano crashes) File->Add/Remove Files-> Add File-....

3. Import calibration tables (~/Documents/X-shooter/A1835/GEN_CALIB/proc) from File->Add/Remove Files-> Add File-....

4. Import calibration files (if it is not in your data files) go to http://archive.eso.org/eso/eso_archive_main.html choose the dates when you data have been taken and mark window CALIB or choose the Data Type

5. Follow reduction cascade by selecting required files (remember the '?' mark next to the file in recipe tables means that the file is optional) and running each recipe Selected files-> To recipe->..

6.In each recipe window set the path for the products of gasgano in window titled "Product Root Directory"

7. Execute the recipes by pressing "Execute"

Reduction cascade

  • (OPTIONAL) Run the recipe xsh_lingain on a set of linearity frames

    • LINEARITY_NIR_ON

    • LINEARITY_NIR_OFF

in order to determine the map of non linear pixels . All the available input frames should be used to better sample the photon transfer curve (usually 40 ON frames and 40 OFF frames). In UVB and VIS arm this step may be skipped, as the number of non linear bad pixels is negligible. The linearity test are done rearlly search in archive for whole year.

Xshooter group said it was optional to do linearity corrections.

  • Build the master bias frame MASTER_BIAS_ARM with the recipe xsh_mbias from a set of raw bias frames. This applies only to VIS and UVB arms. Remeber to sum up BIAS with the same readout mode 100k or 400k and the same binning

    • BP_MAP_NL_VIS -OPTIONAL

    • BIAS_ARM

  • Build the master dark frame MASTER_DARK_ARM with the xsh_mdark from a set of raw dark frames. This applies mainly to NIR arm as in VIS and UVB arms the contribution from the dark current emission is negligible (In Calibration directory there are two MASTRE_BP... both gives identical results)

    • DARK_NIR

  • Generate the guess order ORDER_TAB_GUESS_ARM with xsh_predict from a format- check frame FMTCHK_ARM, a reference list of arc lines ARC_LINE_LIST_ARM and a reference spectral format table SPECTRAL_FORMAT_TAB_ARM. Additional optional inputs are the master bias MASTER_BIAS_ARM and the master dark MASTER_DARK_ARM.

  • Refine the order guess table ORDER_TAB_CENTR_ARM into an order table with xsh_orderpos from an order definition frame ORDERDEF_ARM obtained by illuminating the X-Shooter pinhole with a continuum lamp. Additional required inputs are a reference spectral format table SPECTRAL_FORMAT_TAB_ARM and the guess order table (ORDER_TAB_GUESS_ARM) and in UVB/VIS arm a master bias MASTER_BIAS_ARM. Additional optional input is the master dark MASTER_DARK_ARM.

  • Build the master flat frame MASTER_FLAT_SLIT_ARM and the order tables tracing the flat edges ORDER_TAB_EDGES_SLIT_ARM with the recipe xsh_mflat from a set of raw flat frames FLAT_SLIT_ARM. Additional required inputs are the order table ORDER_TAB_CENTR_ARM and a reference spectral format table SPECTRAL_FORMAT_TAB_ARM and in UVB/VIS arm a master bias MASTER_BIAS_ARM. Additional optional input is the master dark MASTER_DARK_ARM.

  • Determine a table with the dispersion solution coefficients DISP_TAB_ARM and the 2D instrument bidimensional mapping described by an optimized model configuration file (XSH_MOD_CFG_OPT_2D_ARM) in physical model mode using the recipe xsh_2dmap by reducing a multi-pinhole frame WAVE_ARM. MARK MODEL-COMPUTE-MAP IN SETTINGS (TO GET THE DISP_TAB)!!!

  • Determine the instrument response in stare mode RESPONSE_ORDER1D_SLIT_ARM, RESPONSE_MERGE1D_SLIT_ARM and telescope+instrument+detector efficiency EFFICIENCY_ARM with the recipe xsh_respon_slit_stare from a flux standard star observation STD_FLUX_STARE_ARM The instrument response and efficiency are computed only if the observed standard star is listed in the catalog of reference flux standard stars. In this case also flux calibrated merged 1D and 2D spectra are generated.

  • Or determine the response in slit nodding mode RESPONSE_ORDER1D_SLIT_ARM, RESPONSE_MERGE1D_SLIT_ARM by reducing flux standard frames FLUX_STD_SLIT_NOD_ARM with the recipe xsh_respon_slit_nod.

    • Reduce science data in slit stare mode OBJECT_SLIT_STARE_ARM with the recipe xsh_science_slit_stare . Particularly in NIR arm is important to provide in input also the bad pixel map MASTER_BP_MAP_ARM.

    • If the user provides the instrument response table RESPONSE_MERGE1D_SLIT_ARM, and the atmospheric exctinction table ATMOS_EXT_ARM, the merged spectra (1D and 2D) are calibrated in flux units. ADD RESPONSE_SLIT_ARM INSTEED TO RESPONSE_SLIT_MERGED1D_ARM!!!! Or if you do not have it skip the response!!!!!

  • You have submitted OBs with the

    • xsh_scired_slit_stare - for: A1835_2, AC114_2, AC114_3

    • xsh_scired_slit_offset - for the rest you use this mode but insteed you should use this one xsh_scired_slit_nod

  • Now you have to fix the header of all SKY_SLIT_ARM frames changing the CLASSIFICATION to OBJECT_SLIT_OFFSET_ARM

  • You can fix header by opening the frame in the VI editor, but remember that the length of the keyword should be the same so make sure you put the correct number of white spaces, run vi command: :%s/'SKY '/'OBJECT '/g