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EOS P96 User Manual

The x-shooter user manual provides extensive information on the technical characteristics of the instrument, its performances, observing and calibration procedures and data reduction.
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European Organisation
for Astronomical
Research in the
Southern Hemisphere
VERY LARGE TELESCOPE
Prepared: Christophe Martayan, originally written by Joël Vernet & Elena Mason
Name
Approved: Andreas Kaufer, originally approved by Sandro D'Odorico
Name
Released: Christophe Dumas
Name
ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
Organisation Européenne
pour des Recherches
Astronomiques
dans l'Hémisphère Austral
X-shooter
User Manual
Doc. No.: VLT-MAN-ESO-14650-4942
Issue: P96
Date: 24.06.2015
Date
Date
Date
Europäische Organisation
für astronomische
Forschung in der
südlichen Hemisphäre
Signature
Signature
Signature

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Summary of Contents for EOS P96

  • Page 1 Austral südlichen Hemisphäre VERY LARGE TELESCOPE X-shooter User Manual Doc. No.: VLT-MAN-ESO-14650-4942 Issue: P96 Date: 24.06.2015 Prepared: Christophe Martayan, originally written by Joël Vernet & Elena Mason Name Date Signature Approved: Andreas Kaufer, originally approved by Sandro D’Odorico...
  • Page 2 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 2 of 161 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 3 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 3 of 161 CHANGE RECORD ISSUE DATE SECTION/PARA. REASON/INITIATION AFFECTED DOCUMENTS/REMARKS 13.01.06 FDR version: Table of Content prepared by Céline Péroux 14.08.08 PAE version prepared by Joël Vernet 01.03.09 First release prepared by Joël Vernet, with contributions by Elena Mason 01.07.09...
  • Page 4 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 4 of 161 25.08.2010 CMa, sections 2.4.7 and 26.08.2010 2.4.8, 2.4.9, 4.4, 4.7, 4.8 added. Sections 2.2.1, 3.2, 4.5.2, 4.6, 5.1.1, 5.1.2 modified. Figure added in 5.1.1, Table 11 updated, old Table 3 removed. + modified structure of the sections 27.02.2011 Modified sects.
  • Page 5 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 5 of 161 20.02.2012 Modified sections: 2.2.1.4, DIT of 1800s with JH slits, 03.04.2012 2.2.4.5, 2.4.3, 3.4.3, 4.1.2, TCCD limiting magnitudes + 5.1, 5.4, Table 16 revised direct acquisition. Telluric std star observations, Clarification of 2.2.4.3 (new NIR slits) minimize 6.1.2...
  • Page 6 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 6 of 161 91/92 10.02.2013 Section 3.2 split in 2: 3.2.1 Sects 3.2.1/3.2.2: main acq 3.2.2 loop and 3.2.2 blind offset New section 3.3 precision New section 1.6 section about examples preparation with p2pp3 especially regarding acqs (direct or blind offsets)
  • Page 7 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 7 of 161 26.02.2014 Minor changes, references to the imaging mode user manual added. New table about the limiting magnitude for a S/N=10 in sec 2.2.1.4. Some details provided for the dichroic dip oscillation, corrected cross-references.

  • Page 8: Table Of Contents

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 8 of 161 TABLE OF CONTENTS Introduction ........................11 Scope ........................12 X-shooter in a nutshell ..................12 Shortcuts to most relevant facts for proposal preparation ........12 List of Abbreviations & Acronyms ................13 Reference Documents ..................14 Acknowledgements ....................15 Contact .........................15 News ........................16 Technical description of the instrument .................17...
  • Page 9 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 9 of 161 2.4.8.1 Backbone flexures ..................60 2.4.8.2 Spectrograph flexures ...................60 2.4.9 Radial velocity accuracy ................60 2.4.10 NIR 11 order vignetting (K band) ..............61 2.4.11 VIS CCD pick-up noise ..................62 2.4.12 NIR –IFU parasitic reflections ................62 2.4.13 UVB/VIS ADCs problem ................63 2.4.14...
  • Page 10 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 10 of 161 Templates reference ................... 116 7.1.1 Orientation and conventions ................ 116 7.1.2 Examples of position angles and offsets ............118 7.1.3 Acquisition templates .................. 120 Slit acquisition templates ..................120 IFU acquisition templates ..................122 7.1.4 Flexure compensation templates that can be used in OBs ......

  • Page 11: Introduction

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 11 of 161 1. Introduction Figure 1: 3D CAD view of the X-shooter spectrograph at the Cassegrain focus of one of the VLT Unit Telescopes. Table 1: X-shooter characteristics and observing capabilities Wavelength range 300-2500 nm split in 3 arms UV-blue arm Range: 300-550 nm in 12 orders...

  • Page 12: Scope

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 12 of 161 1.1 Scope The X-shooter User Manual provides extensive information on the technical characteristics of the instrument, its performances, observing and calibration procedures and data reduction. 1.2 X-shooter in a nutshell X-shooter is a single target spectrograph for the Cassegrain focus of one of the VLT UTs covering in a single exposure the spectral range from the UV to the K band.

  • Page 13: List Of Abbreviations & Acronyms

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 13 of 161 1.4 List of Abbreviations & Acronyms This document employs several abbreviations and acronyms to refer concisely to an item, after it has been introduced. The following list is aimed to help the reader in recalling the extended meaning of each short expression: A&G/AG Acquisition and Guiding...

  • Page 14: Reference Documents

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 14 of 161 1.5 Reference Documents 1. X-shooter Calibration plan, v1.0, XSH-PLA-ESO-12000-0088 2. X-shooter Templates Reference Manual, v0.2, XSH-MAN-ITA-8000-0031 3. X-shooter technical note about the 11 order vignetting in K band 4. X-shooter A&A article: Vernet et al. 2011A&A...536A.105V 5.

  • Page 15: Acknowledgements

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 15 of 161 1.6 Acknowledgements Please if you use XSHOOTER data, cite the following articles: 1. main article: Vernet et al., 2011A&A...536A.105V X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope 2.

  • Page 16: News

    16 of 161 1.8 News -in P96 a new ETC is available using the image quality on the instrument (instrument+telescope+sky contributions) instead of the seeing. However, the seeing is still used as input in V band at the zenith. There is not yet a new sky model available for XSHOOTER and the NIR background is underestimated in K band.

  • Page 17: Technical Description Of The Instrument

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 17 of 161 2. Technical description of the instrument Figure 2: Schematic overview of X-shooter ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...

  • Page 18: Overview Of The Opto-Mechanical Design

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 18 of 161 2.1 Overview of the opto-mechanical design Figure 2 shows a schematic view of the layout of the instrument. It consists of four main components:  The backbone which is directly mounted on the Cassegrain derotator of the telescope.

  • Page 19: The Backbone

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 19 of 161 2.2.1 The Backbone Figure 3: 3D view of a cut through the backbone. 2.2.1.1 The Instrument Shutter and The calibration unit In the converging beam coming from the telescope, the first element is the telescope entrance shutter.

  • Page 20: The Acquisition And Guiding Slide

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 20 of 161 2.2.1.2 The Acquisition and Guiding slide Light coming either directly from the telescope or from the Calibration Unit described above reaches first the A&G slide. This structure allows putting into the beam either: ...

  • Page 21: The Ifu

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 21 of 161 2.2.1.3 The IFU Figure 4: Top: view of the effect of the IFU. The central field is directly transmitted to form the central slitlet (green) while the each lateral field (in blue and red) are reflected toward a pair of spherical mirrors and realigned at the end of the central slice to form the exit slit.
  • Page 22 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 22 of 161 Below is an example of IFU observation of a telluric standard star: Red orders Blue UVB arm Blue orders Red orders Blue VIS arm Blue orders Red orders Blue NIR arm Blue orders Figure 5: IFU telluric standard star (B-type star).

  • Page 23: The Acquisition And Guiding Camera

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 23 of 161 2.2.1.4 The Acquisition and Guiding Camera The A&G camera allows to visually detecting and center objects from the U- to the z-band. This unit consists in:  a filter wheel equipped with a full UBVRI Johnson filter set and a full Sloan Digital Sky Survey (SDDS) filter set.

  • Page 24: The Dichroic Box

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 24 of 161 2.2.1.5 The dichroic box Light is split and distributed to the three arms by two highly efficient dichroic beam splitters. These are the first optical elements encountered by the science light. The first dichroic at an incidence angle of 15˚...

  • Page 25: The Focal Reducer And Atmospheric Dispersion Correctors

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 25 of 161 2.2.1.7 The Focal Reducer and Atmospheric Dispersion Correctors Both UVB and VIS pre-slit arms contain a focal reducer and an ADC. These focal reducer- ADCs consist of two doublets cemented onto two counter rotating double prisms. The focal reducers bring the focal ratio from f/13.41 to ~f/6.5 and provide a measured plate scale at the entrance slit of the spectrographs of 3.91”/mm in the UVB and 3.82”/mm in the VIS.

  • Page 26: Adcs Problems And Disabled Adcs Observing Mode In Slit And Ifu

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 26 of 161 2.2.2 ADCs problems and disabled ADCs observing mode in SLIT and IFU During March to July 2012 the ADCs (atmospheric dispersion correctors) for the UVB and VIS arms in X-shooter have been occasionally failing. Unfortunately the rate of such failures has increased until being daily, leading sometimes to data taken in sub-optimal instrument configuration, which needs to be taken into account when reducing and analyzing such observations.
  • Page 27 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 27 of 161 a) Atmospheric dispersion effect on the XSHOOTER spectra without ADCs The tracking in XSHOOTER is by default 470nm, and The dispersion effect of the atmosphere on XSHOOTER spectra depends on the tracking wavelength used (by default 470nm).
  • Page 28 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 28 of 161 As consequences, in stare mode (object centered in the slit): -if the observation is conducted at airmass 1.2 with the slit angle at parallactic angle, then the drift between the blue and red order spectrum will be of ~1.6” in the UVB arm, ~0.6” in the VIS arm, and ~0.2”...
  • Page 29 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 29 of 161 Nodding mode, AM=1.35 Ratios no ADCs/with ADCs Arm, slit angle Average range UVB parallactic 0.01 0.87 0.87-0.9 UVB perpendicular 0.82 0.56-1.0 0.15 VIS parallactic 0.88 0.82-0.9 0.02 VIS perpendicular 0.11 0.81 0.66-0.99 The measurements were performed on short integration times and if possible in stable conditions of the seeing.
  • Page 30 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 30 of 161 airmass Type of ratio average range 0.19 1.10 45/parall 0.98 0.84-1.0 0.15 1.10 90/parall 0.83 0.74-1.0 1.51 45/parall 0.84 0.56-1.0 0.13 0.26 1.51 90/parall 0.63 0.25-1.0 2.20 45/parall 0.31 0.05-0.64 0.20 2.20 90/parall 0.18...
  • Page 31 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 31 of 161 f) Comparison of observations efficiency between airmasses and slit angles In the following table the efficiency is compared between airmass 1.51 and 1.10 (flux ratio AM=1.51/AM=1.10). Slit angle average range Parallactic 0.89 0.43-1.0 0.16...
  • Page 32 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 32 of 161 At the Cassegrain focus there is no possibility yet to do a secondary guiding. Therefore the evolution of the parallactic angle is not followed during the exposures but the slit is setup at the parallactic angle at the moment of the acquisition.
  • Page 33 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 33 of 161 1 8 0 1 6 0 1 4 0 1 2 0 - 1 0 1 0 0 - 2 0 - 3 0 - 4 0 - 5 0 - 6 0 - 7 0 - 8 0 For example, the parallactic angle changes by ~110 degrees in 1h (1 HA) for declination...
  • Page 34 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 34 of 161 2 .5 - 1 0 - 2 0 - 3 0 - 4 0 - 5 0 1 .5 - 6 0 - 7 0 - 8 0 From this plot about the airmass variation, one can see that for declination +40 degrees, the airmass will change from AM=2.4 to 2.5 in 1h so a relative small change but it means for the UVB arm a dispersion between the blue and red orders of about 5”...

  • Page 35: Detector Qe Curves

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 35 of 161 2.2.3 Detector QE curves 2.2.4 The UVB spectrograph 2.2.4.1 Slit carriage The first opto-mechanical element of the spectrograph is the slit carriage. Besides the slit selection mechanism, this unit consists of a field lens placed just in front of the slit to re- image the telescope pupil onto the spectrograph grating, and the spectrograph shutter just after the slit.

  • Page 36: Optical Layout

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 36 of 161 2.2.4.2 Optical layout Figure 7: The UVB spectrograph optical layout The optical layout of the UVB spectrograph is presented in Figure 7. Light from the entrance slit, placed behind the plane of the figure, feeds a 5˚ off-axis Maksutov-type collimator through a folding mirror.

  • Page 37: Detector

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 37 of 161 2.2.4.3 Detector The UVB detector is a 20484102, 15µm pixel CCD from E2V (type CCD44-82) of which only a 18003000 pixels window is used. The CCD cryostat is attached to the camera with the last optical element acting as a window.
  • Page 38 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 38 of 161 Detector type E2V CCD44-82 MIT/LL CCID 20 substrate removed Hawaii Operating 153 K 135 K 81 K temperature 80% at 320 nm 78% at 550 nm 88% at 400 nm 91% at 700 nm 83% at 500 nm 74% at 900 nm 81% at 540 nm...

  • Page 39: The Vis Spectrograph

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 39 of 161 2.2.5 The VIS spectrograph 2.2.5.1 Slit carriage The slit carriage of the VIS spectrograph is identical to that of the UVB but the available slits are different. All the science observation slits are 11” high and different widths are offered from 0.4”...

  • Page 40: The Nir Spectrograph

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 40 of 161 2.2.6 The NIR spectrograph The NIR spectrograph is fully cryogenic. It is cooled with a liquid nitrogen bath cryostat and operates at 105 K. 2.2.6.1 Pre-slit optics and entrance window After the dichroic box and two warm mirrors M1 (cylindrical) and M2 (spherical, mounted on a tip-tilt stage and used for flexure compensation, see description on p.
  • Page 41 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 41 of 161 With the change of slits, the resolving power is slightly different: They are indicated in the following table 10. Table 9: NIR spectrograph slits and resolving power slit R old slit wheel R new slit wheel 0.4”...
  • Page 42 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 42 of 161 Below one can see flat-field frames for the slits with and without K band blocking filter. ON-OFF Flat field frames for the normal 0.9” NIR slit (top) and for the 0.9” with blocking filter (bottom).
  • Page 43 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 43 of 161 ON-OFF Flat field frames for the normal 0.6” NIR slit (top) and for the 0.6” with blocking filter (bottom). One can easily note that the last orders are cut by the K-band blocking filter. ESO, Karl-Schwarzschild-Str.

  • Page 44: Nir Backgrounds

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 44 of 161 2.2.6.3 NIR Backgrounds The background of the new slits 0.6”JH and 0.9”JH with the blocking filter was compared to the background of the normal slits 0.6” and 0.9”. The table 11 below gives example of the background measurements at different wavelengths for slits with and without filter.
  • Page 45 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 45 of 161 The figures below for the 0.9” and 0.6” slits with/without filter show the different noises at different wavelength taking into account all the sources of background noises: thermal background, RON, sky background, dark current. The black curve corresponds to the RON.
  • Page 46 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 46 of 161 B Backgrounds with 0.6” slits with/without filters a) For 0.6” slit with K-band blocking filter: Unfortunately, the background is always RON limited. b) For normal 0.6” slit without filter: For this slit, the background is RON limited for DIT up to ~360s at wavelength 1682nm and 450s at 1300nm.

  • Page 47: Optical Layout

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 47 of 161 2.2.6.4 Optical layout Figure 8: The NIR spectrograph optical layout. The optical layout of the NIR spectrograph is presented in Figure 8. The conceptual design is the same than for the UVB and the VIS spectrographs. Light entering the spectrograph via the entrance slit and folding mirror M5 feeds an off-axis Maksutov-inspired collimator.

  • Page 48: Detector

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 48 of 161 2.2.6.5 Detector The NIR detector is a Teledyne substrate-removed HgCdTe, 2k2k, 18µm pixel Hawaii 2RG from of which only 1k2k is used. It is operated at 81K. Measured characteristics and performances are given in Table 6. Sample-up-the-ramp (non-destructive) readout is always used.
  • Page 49 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 49 of 161 Red orders Blue UVB arm Blue orders Red orders Blue VIS arm Blue orders Red orders Blue NIR arm Blue orders Figure 10: example of (top), (middle) and (bottom) calibration frames. Strong order curvature and varying slit tilt and scale are clearly visible.
  • Page 50 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 50 of 161 Table 11: X-shooter spectral format. * These orders are cut for the slits with the K band-blocking filter Order Min. wavelength Blaze wavelength Max. wavelength [nm] [nm] [nm] 293.6 312.2 322.3 306.2 325.0 336.2...

  • Page 51: Spectral Format, Resolution And Overall Performances

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 51 of 161 2.3 Spectral format, resolution and overall performances 2.3.1 Spectral format The spectral format of X-shooter is fixed. The spectral ranges on the detector and blaze wavelength for each order are given in Table 11 and an example of ThAr slit frame for each arm is shown Figure 10.

  • Page 52: Spectral Resolution And Sampling

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 52 of 161 2.3.2 Spectral resolution and sampling The user can only affect the spectral resolution through the choice of slit width (and to some extent with the binning in UVB and VIS). The resolution and pixel sampling (without binning) as a function of the slit width is given in Table 12.

  • Page 53: Overall Sensitivity

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 53 of 161 2.3.3 Overall sensitivity The total efficiency has been measured on sky using several standard stars observed during commissioning. Based on these values, the expected limiting AB magnitudes at blaze in 1 hour for a S/N of 10 per spectral bin are given in Figure 12.
  • Page 54 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 54 of 161 UVB arm VIS arm NIR arm wavelength magnitude wavelength magnitude wavelength magnitude 20.5 1001.6 18.1 2377.28 15.5 957.3 19.3 2179.17 16.8 496.8 21.3 904.3 19.9 2011.54 16.8 466.4 21.4 860.2 19.8 1867.86 16.6 438.8...

  • Page 55: Instrument Features And Known Problems To Be Aware Of

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 55 of 161 2.4 Instrument features and known problems to be aware of 2.4.1 UVB and VIS detectors sequential readout UVB and VIS detectors share the same FIERA controller. While both arms can expose simultaneously, readout is done sequentially.
  • Page 56 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 56 of 161 About the UVB CCD, the recent tests show that the detector does not have remnants after arc exposures of 6 to 300s with the 1x1 binning and the normal readout mode, 3s exposure in the 1x2 binning for the normal readout mode, and 1s exposure for the 2x2 binning in the normal readout mode.

  • Page 57: Ghosts

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 57 of 161 2.4.4 Ghosts Spurious reflections from the rear surfaces of the dichroics towards the first surface and back again produce a secondary image of the object on the slit that is displaced from its parent by few arcsec and leads to almost in focus ghost spectra in the bottom part of the spectra.

  • Page 58: Inter-Order Background

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 58 of 161 2.4.5 Inter-order background Inter-order background subtraction is a difficult task, in particular where order spacing is minimum in the red part of the VIS (~4 unbinned pixels). Therefore, whenever a good inter- order background subtraction by the pipeline is important, we recommend not using the 2x2 binning mode.
  • Page 59 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 59 of 161  With the 0.6”JH slit, some low level interferences are visible in the reddest part of the last order. The fringe peak-to-peak difference accounts for 10% of the level in the worse case.

  • Page 60: Nir Detector: Interquadrant Cross-Talk And Electrical Ghosts

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 60 of 161 2.4.7 NIR detector: interquadrant cross-talk and electrical ghosts -The XSHOOTER NIR detector as most of infrared detector suffers from an effect called interquadrant cross-talk. When part of the array is illuminated by a bright object, some other parts are “activated”...

  • Page 61: Nir 11 Th Order Vignetting (K Band)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 61 of 161 2.4.10 NIR 11 order vignetting (K band) The flux in this 11 order decreases towards the top of the order by a factor of ~10% and is due to a bad design of the mask located in front of the NIR array. The same effect is present in the blue part of the 10 order.

  • Page 62: Vis Ccd Pick-Up Noise

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 62 of 161 2.4.11 VIS CCD pick-up noise The pick-up noise in the VIS detector is present in every readout modes (with a deviation from the background level of lower than 0.5%). This pick-up noise is comparable to the pick- up noise measured on the UVES CCD for example.

  • Page 63: Uvb/Vis Adcs Problem

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 63 of 161 2.4.13 UVB/VIS ADCs problem UVB/VIS ADCs intermittently show initialization problems, especially in cold conditions. Since August 2010 a new operational procedure has been implemented to prevent starting science observations with the UVB/VIS ADCs in a wrong position. In the evening at the time of the instrument startup and during the morning calibrations the ADCs are closely monitored to ensure that the systems are working as expected.

  • Page 64: Observing With X-Shooter

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 64 of 161 3. Observing with X-shooter 3.1 Observing modes and basic choices Starting in P93, X-shooter offers three observing modes: SLIT spectroscopy, IFU spectroscopy, and imaging. The spectral format is fixed for both spectroscopic observing modes. The three arms (UVB, VIS and NIR) operate in parallel.

  • Page 65: Target Acquisition

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 65 of 161 3.2 Target acquisition 3.2.1 Acquisition loop Target acquisition for SLIT and IFU modes is almost identical. The main steps of a typical acquisition sequence are the following: 1. Warmup of the lamp for the flexure correction measurement. 2.

  • Page 66: Blind Offset Precisions

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 66 of 161 FITS header keywords HIERARCH ESO SEQ AG XCEN and YCEN record the location of the centre of the SLIT or IFU in the image. 3.2.2 Blind offset precisions For targets fainter than ~22mag (see Table 3) we recommend to perform a blind offset from a reference star.

  • Page 67: Examples Of Obs Preparations/Acquisitions With P2Pp3

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 67 of 161 3.3 Examples of OBs preparations/acquisitions with p2pp3 Note that in SM, our USD colleagues will help you in case of questions regarding the preparation of the OBs. In VM, there is a support from the astronomers at Paranal. 3.3.1 Direct acquisition Choose the acquisition template...
  • Page 68 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 68 of 161 Science template added, here nodding ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 69 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 69 of 161 Informations of the science target in case of direct acquisition: -coordinates RA, DEC -equinox, epoch -proper motions in RA and DEC in arcsec/year -differential velocities in RA and DEC in “/s if any (moving targets) ESO, Karl-Schwarzschild-Str.
  • Page 70 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 70 of 161 The following snapshots are valid for both direct and blind offset OBs. Specify the constraints: Transparency, seeing, etc. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 71 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 71 of 161 If needed, in case of time critical observation, add a constraint in the time interval (range of dates and times). ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 72 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 72 of 161 Only if actually needed you can also define a range of valid sidereal times for the observation of your target. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...

  • Page 73: Blind Offset Acquisition

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 73 of 161 3.3.2 Blind offset acquisition BLIND OFFSET ACQUISITION Specify here in arcsec the blind offsets from the reference/acquisition star to the science target. Here movements from the acquisition star of 35.6” to the west and 20.5”...
  • Page 74 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 74 of 161 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...

  • Page 75: Spectroscopic Observations

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 75 of 161 3.4 Spectroscopic observations 3.4.1 Overview and important remarks 3.4.1.1 Observing modes X-shooter science templates support different observing strategies: staring (commonly used for UV and visible observations), nodding along the slit (classical near-IR observations, for SLIT only), offsetting to a fixed sky position (for extended objects) or lets the user free to choose any sequence of offsets (e.g.

  • Page 76: Staring (Slit And Ifu)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 76 of 161 Example, NDIT=2, DIT=100s,NINT=1 will give 1 averaged exposure. The total integration time will be of 200s. NDIT=1, DIT=100s, NINT=2 will give 2 exposures of 100s each. The total integration time will be of 200s.

  • Page 77: Nodding Along The Slit (Slit Only)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 77 of 161 3.4.4 Nodding along the slit (SLIT only) This corresponds to the standard way of observing in the near-IR primarily aimed at a double pass sky subtraction. The template XSHOOTER_slt_obs_AutoNodOnSlit automatically nods the telescope between two positions (A and B) along the slit. The user defines a Nod Throw and optionally a small jitter box (in the slit direction).

  • Page 78: Fixed Offset To Sky (Slit And Ifu)

    “offset DEC” is the difference delta DEC. 3.4.7 and IFU) templates In P96, 2 new templates called mapping in SLIT and IFU modes will allow the user to define any pattern by providing a list of (cumulative) telescope offsets. This is particularly useful in case one wants to map an object with several slit or IFU positons.

  • Page 79: Observation Strategy, Summary, And Tricks

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 79 of 161 3.5 Observation strategy, summary, and tricks 3.5.1 Instrument setup Observing mode Instrument Readout/binning Slits/filters mode UVB 100k,1x1 STARE UVB 100k,1x2 UVB 100k,2x2 UVB 400k,1x1 UVB, NODDING UVB 400k,1x2 0.5”,0.8”,1.0”,1.3”,1.6”,5” 9999=parallactic UVB 400k,2x2 FIXED-OFFSET SLIT (RRM angle...

  • Page 80: Observation Strategy

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 80 of 161 3.5.2 Observation strategy This section provides basic information for the observations. To better specify the strategy of your observations, you should contact usd-help@eso.org (SM and VM), or discuss it with the Paranal day/night astronomers (in VM).
  • Page 81 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 81 of 161  Extended object (galaxy) or crowded field (globular cluster): -In case of an extended object, let say a galaxy of 25” in the sky or a star in a huge nebula, the use of the SLIT mode if you are interested by the core of the galaxy or by the star is OK.

  • Page 82: Telluric Standard Stars And Telluric Lines Correction (See Also Sect.6.6.1)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 82 of 161  Imaging mode In P93 the imaging mode of XSHOOTER will be offered. It has to be combined to slit or IFU observations for science OBs. The structure of the OB could be like this: Slit acquisition-stare imaging template1 with filter V 4 exposures of 2s- stare imaging template2 with filter I 3 exposures of 1s-slit nodding observations- stare imaging template3 with filter V…...

  • Page 83: Readout Times In The Uvb And Vis Arms: Minimization Of Overheads

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 83 of 161 According to the ETC and measurements, one must not try to observe stars brighter than magnitude 3 because it will lead to saturate the detectors: It is the case of an A0V or O5 or F0 stars observed under a seeing of 0.8”, at an airmass of 1.2, with the slits 0.5”...

  • Page 84: The Xshooter Imaging Mode

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 84 of 161 4. The XSHOOTER imaging mode Main contributors: C. Martayan, A. Mehner, G. Beccari, E. Pena, W. Hummel, A. Modigliani, A. Smette, and the X-shooter IOT Overview X-shooter remains foremost a set of spectrographs, but a simple imaging mode with limited functionalities is offered to the community starting in P93.
  • Page 85 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 85 of 161 Important warning: because the detector is cooled by a Pelletier, it takes time to evacuate the heating towards the cooling pipes that cool down the Pelletier itself. As a consequence, every time a loop is started or the integration time is modified the first exposures will have a higher background and noise than optimal.
  • Page 86 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 86 of 161 Table 1bis: A&G CCD characteristics. Detector type E2V CCD57-10IE Cooling system Pelletier 82 % at 580 nm, 50 % at 380 nm and 820 nm Number of pixels 562x528 Pixel size 13μmx13μm Pixel scale(''/pixel) 0.1744 +/- 0.0016 (since P92 at UT3)
  • Page 87 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 87 of 161 Figure 2bis: A&G CCD quantum efficiency curve The A&G CCD cooling system produces small oscillations of the CCD temperature. Temperature variations affect the dark current level. In case of short exposure times, when the image sampling frequency corresponds to the frequency of the temperature oscillations, this leads to “beats”...
  • Page 88 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 88 of 161 Figure 3: A&G camera filter curves. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 89 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 89 of 161 Table 2bis: A&G CCD zeropoints. ZP XSHOOTER 24.94 27.27 27.20 27.13 26.73 (10/2014) at UT2 from P94 ZP XSHOOTER 24.83 27.91 27.83 27.74 27.36 (11/2013) at UT3 from P92 ZP XSHOOTER 24.95 27.74 27.63...
  • Page 90 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 90 of 161 Stability of the AGCCD The stability of the imaging mode and the AG CCD detector was investigated. Short, medium and long term stability aspects were tested. a) The spectrophotometric standard star GD71 was monitored over 1 hour with exposures every few seconds.
  • Page 91 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 91 of 161 ambient temperature increase or if the temperature is high, the Peltier is not cooled down fast enough and the background/noise structure is higher. However, despite this temporary increase this detector remains the best acquisition detector at Paranal. Calibration plan and observing strategies a) Imaging mode acquisition and exposure times A basic imaging observing block (OB) consists of a slit or IFU acquisition template, followed...
  • Page 92 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 92 of 161 c) Calibration plan The calibration plan is defined below. It may evolve in the next months/periods. Table 6bis: Calibration plan. Type of calibration Template Frequency Day: bias XSHOOTER_img_cal_Dark 10, daily Day: dark XSHOOTER_img_cal_Dark on request, 3x10s monthly Day: linearity...
  • Page 93 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 93 of 161 Distortion map, fringes, and astrometric accuracy Figure 5bis shows the distortion maps of the TCCD with respect to the 2MASS astrometry (Fig. 6bis). Figure 5bis: UBVRI distortion maps magnified x20. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 94 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 94 of 161 Fig.6bis: Distributions in RA and DEC of the difference between 2MASS and the AGCCD astrometry. The difference between 2MASS and the A&G CCD astrometry is ±0.1”. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 95 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 95 of 161 The Fringing maps were obtained with skyflats. The most affected filters are the r', i', z', I. The amplitude peak to peak ranges from 2 % in the r' to 4% in the z' filter. Fig.
  • Page 96 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 96 of 161 Calibration frames overview and examples Figure 8bis: Three color (BVI) image of a galaxy with a supernova (left) and of a small field of 47Tuc (right). Observations were performed in stare mode. More examples are shown in the Messenger article of the XSHOOTER imaging mode.
  • Page 97 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 97 of 161 Figure 9bis: Example of calibration images. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 98 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 98 of 161 Data reduction No pipeline support will be provided for the imaging data as there are lots of tools to reduce imaging data, extract the objects, and do the photometry. Pipeline support will be provided for the detector linearity determination only.
  • Page 99 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 99 of 161 2) Optionally: create the masterdark Same than 1) for combining the images. 3) Create the masterflatfield Same than 1) for combining the images. Determine the count level with the IRAF imstat task. Normalize the image with the imarith task to obtain the master flatfield.

  • Page 100: Instrument And Telescope Overheads

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 100 of 161 5. Instrument and telescope overheads 5.1.1 Summary of telescope and instrument overheads Table 14: overheads Acquisition and setup Telescope pointing, guide star acquisition, 360s start active optics. X-shooter backbone flexure measurement. Interactive acquisition loop See a SLIT: see b...
  • Page 101 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 101 of 161 XSHOOTER_slt_acq_RRM=360+(Tel offset + AG_EXPOSURE)*3+AG_EXPOSURE XSHOOTER_ifu_acq_RRM=360+(Tel offset + AG_EXPOSURE)*3+AG_EXPOSURE if the AG_EXPOSURE time is setup at 1s: XSHOOTER_slt/ifu_acq=360+(15+1)*3+1=409s if the AG_EXPOSURE time is setup at 3mn or 180s: XSHOOTER_slt/ifu_acq=360+(15+180)*3+180=1025s If the AG exposure time is lower than 1s, the wiping time for doing the snapshot takes about 1s, therefore a minimum time of 1s is considered.

  • Page 102: Execution Time Computation And How To Minimize The Overheads

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 102 of 161 5.1.2 Execution time computation and how to minimize the overheads a) Example 1: slit mode, UVB/VIS arms execution time higher than the NIR one An user defines the observation of a star magnitude 15 in V. He uses a direct acquisition.
  • Page 103 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 103 of 161 c) p2pp check: In p2pp the algorithm takes into account the different exposure times and their number, readout times, the acquisition time, and the instrument setups. Note that there is an extra 5s time between the moment of the UVB/VIS arms setup is done and the NIR one is done.

  • Page 104: Calibrating And Reducing X-Shooter Data

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 104 of 161 6. Calibrating and reducing X-shooter data 6.1 X-shooter calibration plan The calibration plan has been revised during P86, P87, P88, P89, it is now implemented as indicated below. A better follow-up of and new long term calibrations have been included. A summary of the calibration plan manual is given in Table 15 and 17.
  • Page 105 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 105 of 161 a: Darks: every day monitoring darks DITxNDITxNEXP of 1sx3x3; 5sx3x3; 300sx1x3; 600sx1x3 are taken. The other darks are taken only if they are science triggered. They are taken at daytime following the science observation as follows: Science of standard Triggered calibrations NDIT...
  • Page 106 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 106 of 161 Table 16: long –term calibration plan Calibration UVB frames VIS frames Frequency Purpose frames 3x1hour monthly DARK_UVB_100k dark 3x1hour monthly DARK_UVB_400k dark 3x1hour monthly DARK_VIS_100k dark 3x1hour monthly DARK_VIS_400k dark 3x1hour monthly DARK_UVB_100k_1x2 dark...

  • Page 107: Wavelength And Spatial Scale Calibration

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 107 of 161 6.2 Wavelength and spatial scale calibration As described in section 2.3.1, the spectral format of X-shooter is relatively complex with highly curved orders, variable line tilt, dispersion and spatial scale along each order. Using just long slit arc spectra is not sufficient because it is essential to also calibrate the change of spatial scale (just measuring the slit height is not accurate enough).

  • Page 108: Flat-Field And Wavelength Calibrations

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 108 of 161 6.3 Flat-field and Wavelength calibrations WARNING: ALL EXPOSURE TIMES WILL BE REVISED TO PROVIDE BETTER CALIBRATION FRAMES. Flatfield spectra allow to correct for the pixel-to-pixel variations in detector sensitivity as a function of impinging wavelength of the light and to correct for the structures introduced by imperfections of the slits.

  • Page 109: Spectroscopic Skyflats

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 109 of 161 6.4 Spectroscopic skyflats It is now possible to request the support astronomers to take spectroscopic skyflats (both slit and IFU modes). They will be taken on the best effort basis. The performed tests show that the slits are uniformly illuminated. ESO, Karl-Schwarzschild-Str.

  • Page 110: Attached Calibrations

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 110 of 161 6.5 Attached calibrations It is possible to include arc and flat calibration in an observing OB. For the selection of offered night time attached calibrations, see Table 40 and following). However, we strongly discourage taking night time attached arcs in the VIS arm (SLIT or IFU) because of remnants caused by a few strong ThAr lines.
  • Page 111 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 111 of 161 spectrum of the hot star. Some hot stars also have emission lines or are in dusty regions. These stars should be avoided. The V-I colour of the star can be used as an indicator of dust.

  • Page 112: Absolute Flux Calibration

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 112 of 161 6.6.2 Absolute flux calibration Spectrophotometric standard stars can be used to obtain the absolute efficiency of the instrument and derive an absolute flux calibration of the science data. These observations are done by the Observatory with the wide 5.0” slit with dedicated templates XSHOOTER_slt_cal_StandardStar and XSHOOTER_ifu_cal_StandardStar.

  • Page 113: The X-Shooter Pipeline

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 113 of 161 6.7 The X-shooter pipeline A new X-shooter pipeline >v2.5.5 will be released soon fixing some bugs and improving the flexures correction and wavelength calibration. The X-shooter pipeline v2.2.0 has been recently released with its REFLEX support. With REFLEX several recipes are user-interactive with displayed plots allowing checking the results on the fly and re-running the recipes with modified parameter values.

  • Page 114: Examples Of Observations With X-Shooter

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 114 of 161 6.8 Examples of observations with X-shooter During this first year of operation, some achievements were done. For example: - galaxies at high redshift (z=7.5) were observed, - highly extinguished stars (Vmag=27) were observed, -GRB host galaxy of R>=24 were observed as well as GRB afterglow of Rmag=23.5.
  • Page 115 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 115 of 161  What is the frequency of the AFC? After 1h, 1h15mn it is necessary to do the measurements and correct the instrument flexures. Only the backbone flexures are actually measured, not the internal spectrograph flexures.

  • Page 116: Reference Material

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 116 of 161 7. Reference material 7.1 Templates reference In the following sections all the currently defined X-shooter templates are listed with their free and fixed parameters. When using the P2PP tool the user has to fill only the fields (keywords) shown on white background colour in the following tables.

  • Page 117: Doc: Vlt-Man-Eso

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 117 of 161 Figure 19: The slit coordinate system and correspondence between object position in the slit and position on the spectrum for each arm. An object at positive x (black star top panel) produces spectra placed as illustrated in the bottom panels.

  • Page 118: Examples Of Position Angles And Offsets

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 118 of 161 7.1.2 Examples of position angles and offsets TEL.ROT.OFFANGLE is the keyword in the acquisition templates to set up the slit position angle on sky. A value of 9999 (default) means that the parallactic angle is used. The parallactic angle is not followed during the exposure, the system uses the parallactic angle at the start of the OB.
  • Page 119 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 119 of 161 i) Examples of offsets As indicated a positive offset in the x or y direction will move the object in direction of +x and +y axis. The first example with PA=0 degree shows the results of a positive offset in +x. The object/star moves in the direction of the +x axis and the slit moves in the –x axis.

  • Page 120: Acquisition Templates

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 120 of 161 It is important to note that the offsets in all templates are offsets on sky as in other Paranal instruments. They are computed as follows: “offset RA= (delta RA)xcos(DEC), and offset DEC= delta DEC”. It is also important to take into account the proper motions of the objects.
  • Page 121 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 121 of 161 Table 19: User defined and fixed keywords for XSHOOTER_slt_acq_rmm. XSHOOTER_slt_acq_rrm Keyword Range Default Value Label in P2PP Free parameters SEQ.RRM.REGISTER T, F Register system SEQ. RRM.VISITOR T, F Allow RRM activation in visitor mode TEL.TARG.DELTA 000000.000...

  • Page 122: Ifu Acquisition Templates

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 122 of 161 IFU acquisition templates Table 20: User defined and fixed parameters for XSHOOTER_ifu_acq. XSHOOTER_ifu_acq Keyword Range Default Value Label in P2PP Free parameters TEL.TARG.ALPHA 000000.000 Target RA TEL.TARG.DELTA 000000.000 Target DEC TEL.TARG.EQUINOX -2000..3000 2000 Equinox...
  • Page 123 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 123 of 161 Table 21: User defined and fixed parameters for XSHOOTER_ifu_acq_rrm. XSHOOTER_ifu_acq_rrm Keyword Range Default Value Label in P2PP Free parameters SEQ.RRM.REGISTER T, F Register system SEQ. RRM.VISITOR T, F Allow RRM activation in visitor mode TEL.TARG.ALPHA 000000.000...

  • Page 124: Flexure Compensation Templates That Can Be Used In Obs

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 124 of 161 7.1.4 Flexure compensation templates that can be used in OBs Two new templates are available in order to provide the possibility for the user to do additional flexure compensations in case of a long OB (longer than 1h-1h15mn). This new kind of template can be inserted between 2 science templates for instance.
  • Page 125 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 125 of 161 Table 23: Parameters for synchronized stare UVB, VIS and NIR observations with the template XSHOOTER_slt_obs_StareSynchro. XSHOOTER_slt_obs_StareSynchro Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME see Table 4 1.0x11 UVB slit INS.OPTI4.NAME see Table 7 0.9x11...
  • Page 126 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 126 of 161 Table 24: Parameters for the template XSHOOTER_slt_obs_AutoNodOnSlit.It allows to observe nodding along the slit. The values of the nodding and jitter correspond to the width of the box, float values are allowed. XSHOOTER_slt_obs_AutoNodOnSlit Keyword Range...
  • Page 127 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 127 of 161 Table 25: Parameters for the template XSHOOTER_slt_obs_FixedSkyOffset.It allows to alternate object and sky observations by couple. XSHOOTER_slt_obs_FixedSkyOffset Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME see Table 4 1.0x11 UVB slit INS.OPTI4.NAME see Table 7...
  • Page 128 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 128 of 161 Table 26: Parameters for the template XSHOOTER_slt_obs_GenericOffset.It allows to decide the sequence of offsets and object or sky observations but with some restrictions concerning the number of exposures per position and exposure times. XSHOOTER_slt_obs_GenericOffset Keyword Range...

  • Page 129: Ifu Observations

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 129 of 161 IFU observations Table 27: User defined and fixed parameters for IFU observations in stare mode with the template XSHOOTER_ifu_obs_Stare. XSHOOTER_ifu_obs_Stare Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s) DET1.READ.CLKDESCR see Table 5...
  • Page 130 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 130 of 161 Table User defined fixed parameters template XSHOOTER_ifu_obs_FixedSkyOffset. It allows to alternate object and sky observations taking the sky at fixed postion. XSHOOTER_slt_ifu_FixedSkyOffset Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s)
  • Page 131 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 131 of 161 Table User defined fixed parameters template XSHOOTER_ifu_obs_GenericOffset. See as well the mapping template. XSHOOTER_ifu_obs_GenericOffset Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s) DET1.READ.CLKDESCR see Table 5 100k/1pt/hg UVB readout mode DET2.WIN1.UIT1...

  • Page 132: Night-Time Calibration Templates

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 132 of 161 7.1.6 Night-time Calibration Templates Spectro-photometric Standard Stars Table 31: User and fixed keywords for XSHOOTER_slt_cal_SpecphotStdStare. The template is identical to that for slit observation in stare mode except for some of the default parameters. XSHOOTER_slt_cal_SpecphotStdStare Keyword Range...
  • Page 133 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 133 of 161 Table 32: User defined and fixed parameters for XSHOOTER_slt_cal_SpecphotStdOffset. The template is identical to that for alternate object-sky slit observations except for some of the default parameters. XSHOOTER_slt_cal_SpecphotStdOffset Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME...
  • Page 134 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 134 of 161 Table 33: User defined and fixed parameters for XSHOOTER_slt_cal_SpecphotNodding. The template is identical to the XSHOOTER_slt_obs_AutoNodOnSlit one XSHOOTER_slt_cal_SpecphotNodding Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME see Table 4 5.0”x11”...
  • Page 135 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 135 of 161 Table 34: User defined and fixed parameters for XSHOOTER_ifu_cal_SpecphotStdStare. The template is identical to that for the IFU observations in stare mode. XSHOOTER_ifu_cal_SpecphotStdStare Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s)
  • Page 136 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 136 of 161 Table 35: User defined and fixed parameters for XSHOOTER_ifu_cal_SpecphotStdOffset. The template is identical to the XSHOOTER_ifu_obs_FixedSkyOffset. XSHOOTER_ifu_cal_SpecphotStdOffset Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s) DET1.READ.CLKDESCR see Table 5 100k/1pt/hg UVB read-out mode...

  • Page 137: Telluric Standards

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 137 of 161 Telluric standards Table 36: User and fixed keywords for XSHOOTER_slt_cal_TelluricStdStare. The template is identical to the XSHOOTER_slt_obs_Stare one. XSHOOTER_slt_cal_TelluricStdStare Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME see Table 4 1.0x11 UVB slit INS.OPTI4.NAME...
  • Page 138 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 138 of 161 Table 37: User defined and fixed parameters for SHOOT_slt_cal_TelluricStdNod. The template is identical to the XSHOOTER_slt_obs_AutoNodOnSlit one. XSHOOTER_slt_cal_TelluricStdNod Keyword Range Default Value Label in P2PP Free parameters INS.OPTI3.NAME see Table 4 1.0x11 UVB slit INS.OPTI4.NAME...
  • Page 139 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 139 of 161 Table 38: User defined and fixed parameters for SHOOT_ifu_cal_TelluricStdStare. The template is identical to XSHOOTER_ifu_obs_Stare. XSHOOTER_ifu_cal_TelluricStdStare Keyword Range Default Value Label in P2PP Free parameters DET1.WIN1.UIT1 0..36000 UVB exposure time (s) DET1.READ.CLKDESCR see Table 5 100k/1pt/hg...

  • Page 140: Attached Night Calibrations: Must Be Taken After A Science Template

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 140 of 161 Table 39: User defined and fixed parameters for SHOOT_ifu_cal_TelluricStdOffset. The template is identical to XSHOOTER_ifu_obs_FixedSkyOffset. Be careful, the offsets in RA and DEC are setup by default to 1”. XSHOOTER_ifu_cal_TelluricStdOffset Keyword Range Default Value Label in P2PP...
  • Page 141 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 141 of 161 Table 41: Parameters for the template XSHOOTER_slt_cal_UVBLampFlatAtt. XSHOOTER_slt_cal_UVBLampFlatAtt Keyword Range Default Value Label in P2PP Free Parameters DET1.WIN1.UIT1.HIGHF 0..36000 exposure time (High Flat) DET1.WIN1.UIT1.LOWF 0..36000 exposure time (Low Flat) DET2.READ.CLKDESCR see Table 5 VIS readout mode SEQ.NEXPO.HIGHF 0..100...
  • Page 142 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 142 of 161 Table 44: Parameters for the template XSHOOTER_ifu_cal_UVBVisArcAtt. XSHOOTER_ifu_cal_UVBVisArcsAtt Keyword Range Default Value Label in P2PP Free Parameters DET1.WIN1.UIT1 0..36000 UVB exposure time DET1.READ.CLKDESCR see Table 5 UVB readout mode DET2.WIN1.UIT1 0..36000 VIS exposure time DET2.READ.CLKDESCR see Table 5...

  • Page 143: Arcs Multi-Pinhole: 2D Wave Maps (Wavelength Calibration)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 143 of 161 Table 47: Parameters for the template XSHOOTER_ifu_cal_NIRLampFlatAtt. XSHOOTER_ifu_cal_NIRLampFlatAtt Keyword Range Default Value Label in P2PP Free Parameters DET3.DIT 0..36000 NIR exposure time (DIT) DET3.NDIT 0..20 sub- integrations SEQ.NEXPO 0..100 No. of exposures Fixed Value INS.MODE IFUSPEC,SLITSPEC...
  • Page 144 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 144 of 161 Table 50: User and fixed keywords for XSHOOTER_slt_cal_NIRArcsMultiplePinhole. XSHOOTER_slt_cal_NIRArcsMultiplePinhole Keyword Range Default Value Label in P2PP DET3.DIT 0..36000 NIR exposure time DET3.NDIT 1..20 Number of DITs SEQ.NEXPO 0..100 NIR No. of exposures Fixed Value INS.MODE SLITSPEC,IFUSPEC...

  • Page 145: Daytime Calibration Templates

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 145 of 161 7.1.7 Daytime Calibration templates Slit and IFU arc lamp calibrations (resolution, tilt) Table 48: User and fixed keywords for XSHOOTER_slt_cal_UVBVisArcs. XSHOOTER_slt_cal_UVBVisArcs Keyword Range Default Value Label in P2PP Free Parameters INS.OPTI3.NAME see Table 4 1.0x11 UVB slit...

  • Page 146: Flatfield (Pixel Response, Orders Localization)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 146 of 161 Table 50: User and fixed keywords for XSHOOTER_ifu_cal_UVBVisArcs XSHOOTER_ifu_cal_UVBVisArcs Free Parameters Keyword Range Default Value Label in P2PP DET1.WIN1.UIT1 0..36000 UVB Exposure Time DET1.READ.CLKDESCR see Table 5 400k/1pt/lg UVB readout mode DET2.WIN1.UIT1 0..36000 VIS Exposure Time...
  • Page 147 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 147 of 161 Table 53: User and fixed keywords for XSHOOTER_slt_cal_VISLampFlat XSHOOTER_slt_cal_VISLampFlat Free Parameters Keyword Range Default Value Label in P2PP INS.OPTI4.NAME see Table 4 0.9x11 VIS slit DET2.WIN1.UIT1 0..36000 VIS Exposure Time DET2.READ.CLKDESCR see Table 5 100k/1pt/hg VIS readout mode...
  • Page 148 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 148 of 161 Table 56: User and fixed keywords for XSHOOTER_ifu_cal_VISLampFlat XSHOOTER_ifu_cal_VISLampFlat Free Paramters Keyword Range Default Value Label in P2PP DET2.WIN1.UIT1 0..36000 12.2 VIS Exposure Time DET2.READ.CLKDESCR see Table 5 100k/1pt/hg VIS readout mode SEQ.NEXPO 0..100 VIS No.

  • Page 149: Format Check (1 Guess Of Wavelength Solution)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 149 of 161 Format check (1 guess of wavelength solution) Table 58: User and fixed keywords for XSHOOTER_slt_cal_UVBVisArcsSinglePinhole XSHOOTER_slt_cal_UVBVisArcsSinglePinhole Free Parameters Keyword Range Default Value Label in P2PP DET1.WIN1.UIT1 0..36000 UVB Exposure Time DET1.READ.CLKDESCR see Table 5 400k/1pt/lg UVB readout mode...

  • Page 150: Arcs Multi-Pinhole: 2D Wave Maps (Wavelength Calibration)

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 150 of 161 Table 61: User and fixed keywords for XSHOOTER_slt_cal_VISLampFlatSinglePinhole. XSHOOTER_slt_cal_VISLampFlatSinglePinhole Free Paramters Keyword Range Default Value Label in P2PP DET2.WIN1.UIT1 0..36000 VIS exposure time DET2.READ.CLKDESCR see Table 5 400k/1pt/lg VIS readout mode SEQ.NEXPO 0..100 No.

  • Page 151: Detector Calibrations

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 151 of 161 Detector calibrations Table 65: User and fixed keywords for XSHOOTER_gen_cal_Bias XSHOOTER_gen_cal_Bias Free Parameters Keyword Range Default Value Label in P2PP DET1.READ.CLKDESCR see Table 5 100k/1pt/hg UVB read-out mode DET2.READ.CLKDESCR see Table 5 100k/1pt/hg VIS read-out mode SEQ.NEXPO.UVB...
  • Page 152 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 152 of 161 Table 68: User and fixed keywords for XSHOOTER_gen_cal_DarkUVBVIS template. This template allows to run biases for the UVB/VIS arms simultaneously of darks in the NIR arm. Table 69: New multi-order definition template XSHOOTER_slt_cal_MultipleOrderDef running for multi-pinholes with FF lamps and giving order definition for each pinhole of the row.
  • Page 153 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 153 of 161 Table 70: Template for taking detector FF and biases for the linearity measurements of the detectors. ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...

  • Page 154: Imaging Mode Templates Manual

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 154 of 161 7.1.8 Imaging mode templates manual a) Approved template combinations XSHOOTER_img_acq+ VM only XSHOOTER_img_obs, XSHOOTER_img_obs_GenericOffset XSHOOTER_img_acq+ XSHOOTER_img_cal_phot and/or XSHOOTER_img_cal_dist XSHOOTER_slt_acq* + 1 SLT science or std template Possibility to add: XSHOOTER_img_obs, XSHOOTER_img_obs_GenericOffset, XSHOOTER_img_cal_phot, XSHOOTER_img_cal_dist XSHOOTER_ifu_acq* + 1 IFU science or std template Possibility to add:...
  • Page 155 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 155 of 161 b) Template description NIGHTIME IMAGING TEMPLATES: Imaging acquisition template (also allows blind offset) ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 156 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 156 of 161 Special imaging acquisition template for taking imaging skyflats. This template presets the telescope but does not request any active optics or guiding. This template can be combined with the skyflats template: XSHOOTER_img_cal_Flat.tsf ESO, Karl-Schwarzschild-Str.
  • Page 157 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 157 of 161 Science STARE imaging observation Science Generic-OFFSET imaging observation ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany...
  • Page 158 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 158 of 161 Calibration template for observation of standard field for distortion map (same functionality as the science imaging generic-offset template) Calibration template for observation of standard fields for zeropoint determination (same functionality as the science imaging generic-offset template) ESO, Karl-Schwarzschild-Str.
  • Page 159 Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 159 of 161 DAYTIME IMAGING TEMPLATES Calibration template for biases (DET4.WIN1.UIT1 = 0 s) and darks (DET4.WIN1.UIT1 > 0 s) Calibration template for twilight flatfields Calibration template to measure the detector gain and linearity ESO, Karl-Schwarzschild-Str.

  • Page 160: Slit Masks

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 160 of 161 7.2 Slit masks 7.2.1 UVB Table 71: full description of the UVB slit mask Position Size Physcal size (µm) Purpose 0.5”  pinhole 126  hole 1256  2763 5”11” slit 402 ...

  • Page 161: Nir

    Doc: VLT-MAN-ESO-14650-4942 Issue Date 24.06.2015 Page 161 of 161 7.2.3 NIR Table 73: full description of the new NIR slit mask Position Size Physcal size (”) Purpose 0.5”  pinhole 0.490 5”11” slit 5.004 SCI / CAL 0.917 SCI / CAL 0.9”11”...

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