EUROPEAN SOUTHERN OBSERVATORY

La Silla Science Operations: NTT

EMMI	New RED CCD Commissioning report and notes for the observer

General		First light: M8, or the Lagoon Nebula in Sagitarius. This is a false color V (blue), R (green), I (red) composite, 60s per filter. (full size). (pic Vanzi and the commissioning team).
In April 2002, the good old TEK CCD of the Red arm of EMMI has been replaced by a 2x1 mosaic of new generation MIT 2kx4k chips. This page lists the characteristics of EMMI with that new chip almost in real time as we get them. This information will then drift into the main pages and into the EMMI manual. In the meantime, THIS is the reference. This document wll also be eventually converted into a formal commissioning and -hopefully- acceptance report. A quick reference guide is available for the inpatient and/or experienced EMMI users
News
This page lists the info on the new CCD almost in real time as we get it. Be sure to re-check it every time you deal with EMMI, until the new manuals are on-line. May 16: the overscans were adjusted to take the gap geometry properly into account May 15: very high wind. We did not open. May 14: on-sky commissioning, night 2. Thick fog and high wind.Weather improved shortly: acquisition templates were commissioned, and many throughputs were measured. May 13: on-sky commissioning, night 1. It is raining. May 7-12: off-line commissioning April 2002: TEK removed, MIT installed

Table of Content

Commissioning

Introduction
- Purpose and scope
- Documents
CCD: bias, dark, gain, RON
- CCD geometry
- Read-out modes
RILD - Imaging
- Astrometry, field of view,orientation etc
- Flat fields
- Photometry and throughputs
RILD - Low resolution spectroscopy (Grisms)
- Wavelength range, resolution, etc
- Wavelength calibration and lamps
- Wavelength Atlas
- Throughputs
REMD-spec - Medium Resolution Spectroscopy (Gratings)
- Wavelength range, resolution, etc
- FlatFields
- Wavelength Atlas
REMD-ech - High Resolution Spectroscopy (Echelle)
FITS Files and related tips and hints
Oberving template and instrument package

Acceptance

Commissioning

Introduction

Purpose and scope

This document lists the characteristics of the new EMMI Red detector, as measured during the commissioning period of 2002-May. It is a "live" document, wich is often updated as more information becomes available. It will eventually be formalized into a Commissionning Report, and the information will be passed to the other web pages and instrument manual.

The commissioning team was constitued by D.Sluse, C.Foellmi, P.LeSaux, M.Pizarro, A.Sanchez, M.Castillo, J.Miranda, D.Castex, K.Aubel, L.Vanzi from the NTT Team, P.Sinclaire and A.Pizarro from Detector Team, B.Lopez, J.C.Guzman, J.Ibsen for Software, choregraphy by O.Hainaut.

Document

The following documents are used for the commissioning or referenced in this document.

1. LSO-MAN-ESO-40100-0001/4.4 EMMI User's Manual, Gonzalez et al
2. N-PLA-ESO-109-076 NTT Upgrade - EMMI Commissioning Plan, Martin
3. LSO-TRE-ESO-40200-1036 Test and Technical Time Report: Period 36, Oct.22-24, 1999, Hainaut
4. Reflecting Telescope Optics, R.N.Wilson, Springer (Vol 1 and 2)
5. LSO-PLA-ESO-40400-0001/0.93 EMMI Red CCD Upgrade Plan, Hainaut and d'Odorico.
6. VLT-INS-96-0142, Repair of EMMI Red Camera: image quality, Dekker and Buzzoni

CCD, bias and dark

Hardware and Geometry

Figure: CCD orientation in the various modes (also in PS with a better resolution)

The new EMMI Red detector is a 2x1 mosaic of 2kx4k MIT/LL, thinned CCDs, known as CCID20-14-5-3, nicknamed "Michele" and "Zeus". The new detector system is basically a copy of the FORS2 upgrade. The 15micron pixel (0.1665", cf below) match well the resolution of the EMMI-Red optics (0.21", [6]). The mosaic is controlled by FIERA which, together with the ATM connection between the CCD controller and the instrument workstation, ensure a very small overhead.

The two chips are mounted side by side. Each chip uses two independent amplifiers. The resulting frame therefore contains 4 independent sub images (which are stored as extensions in the FITS frame, cf FITS section below). The geometry and name of the subframes are listed in the table below. Refer to the Astrometry section for the accurate relative positioning of the chips.

	Michele Left: Slave CCD, Nr1		Zeus Right: Master CCD, Nr0
Amplifier	A	B	C	D
"Detector"	2B	2A	1B	1A
FITS Extension	c	b	a	-
First X Pixel (= START of each region) (values as of 2002-05-18)	1.	1039.	2077.	3115.

Gap: X=2073-2120 (incl) are overscan, introduced to match the physical gap between the CCD. Refer to the "Astrometry" section for details.
Distance from the mean plane of the camera flange to the mean plane of the CCD: 12.02+/-0.005micron (Deiries/Sinclaire lab measurement)
Planeity (Deiries/Sinclaire lab measurement):
- tilt of the mosaic to the camera flange :
  - x: -0.47 mrad
  - y: -0.37 mrad
- Deviation from planearity: 38micron peak-to-valley

Read-Out Modes

The mosaic is offered exclusively in the following modes

Read-out speed:
- "Slow", or 100Kps (kilo pixel/sec) low read-out-noise for spectroscopy
- "Normal" or 225kps, normal read-out-noise, all purpose
- "Fast" or 625kps, super fast read-out, higher noise, suitable only for acquisition, tests, etc.
Note that the read-out mode indicated in the header always state "Normal". The information about the read out speed is in ESO_DET_READ_CLOCK, which contains the speed in kps. The chips currently present a low level pick-up noise (that appears as "Wiggles" in the bias), which is tracked to a grounding conflict. This will be eliminated.
Binning: 1x1 and 2x2 exclusively. 2x2 (=0.33"/pix) is recommended for most applications.
Window: full mosaic only (NO subwindow allowed)

Table : value of the bias, gain (e/ADU) and RON (e).

CCD subchip		c		b		a		-
		1x1	2x2	1x1	2x2	1x1	2x2	1x1	2x2

Slow=100kps	bias	198	199	199	200	197	198	197	199
	gain	1.35	1.27	1.31	1.28	1.37	1.32	1.34	1.31
	RON	3.90	3.79	3.70	3.57	4.04	3.48	3.68	3.35

Normal=225kps	bias	198	189	199	196	198	194	199	190
	gain	1.35	1.32	1.31	1.29	1.36	1.33	1.33	1.31
	RON	7.64	6.59	6.94	8.92	7.75	9.25	7.01	9.45

Fast=625kps	bias	176	193	183	197	185	199	184	204
	gain		1.46		1.42		1.48		1.50
	RON	39.33	21.8	37.4	20.17	56.6	28.4	37.3	19.8

Dark current

Dark current has been measured on a composite 3h exposure taken in "Slow" mode. Average dark current is 0.3e-/h/pix, with some peaks at 1.5e-/h/pix, and few hot pixels above 5e-/h/pix (ref: com. 2002-05-18: CcdDark).

Linearity

The 4 sub-CCDs have been tested for linearity in the 6 read-out modes. The linearity is better than 0.5% over the full dynamical range (tests by Detector Team, confirmed by routine tests by NTT Team). More information will be available on-line on the detector page, as soon as the HTML interface is configured for the new set-up.

Read-Out Times

The table below lists

the read-out times (including physical read-out and transfer to the instrument workstation via the ATM direct link, and
the total exposure time including minimum overhead i.e. electronics and software overhead, but no hardware overhead (i.e. assuming the instrument is already set-up in the corresponding mode), for a 0sec exposure time. Compare these times with the equivallent values for the old chip (90 to 180sec!)

Table: Read-out times and total software overhead (s)

Mode1x1		2x2
Slow	43.9 / 48	11.7 / 18
Normal	20.1 / 24	5.7 / 18
Fast	9.9 / 18	3.4 / 18

Quantum Efficiency

The figure below displays the quantum efficiency of a MIT/LL ("Michelle") similar to those installed in EMMI-Red, together with that of the former Tek CCD (from [5]). Figure: CCD Quantum efficiencies (ps)

Imaging

Astrometry

Most of the information is summarized graphically in the figure below.

Pixel size: 0.166 5 +/- 0.000 6 arcsec/pix
Orientation (with Rotator offset=0): North = Down, East = Right, with an error of 0.04deg.
Field of view:
- X: [830,4105] = 3275pix = 545" = 9.1' in the E-W direction
- Y: [220,3800] = 3580pix = 596" = 9.9' in the N-S direction
- Gap: X=2059-2068 are overscan as of 2002-05-15
Astrometric transformation and distorsion: (as of 2002-05-12)
- Right (Master) chip
  - d(RA) = cst + 0.046 274 x + 0.000 144 y + 0.000 002 xy + 0.000 024 x^2 -0.000 014 y^2
  - d(Dec) = cst -0.000 029 x -0.046 179 y - 0.000 044 xy +0.000 039 x^2 -0.000 019 y^2
- Left (Slave) chip:
  - d(RA) = cst + 0.046 489 x + 0.000 139 y + 0.000 000 xy -0.000 018 x^2 -0.000 005 y^2
  - d(Dec) = cst -0.000 050 x - 0.046 299 y -0.000 009 xy + 0.000 004 x^2 -0.000 003 y^2
  d(Ra) and d(Dec) are in degrees, x, y in (unbinned) pixel.
CCD translation:
- as of 2002-05-15, there is a translation of the "slave" chip with respect to the master chip:
  - X(master) - X(slave) = 27.0 pix = 4.5"
  - Y(master) - Y(slave) = -2.6 pix = 0.43"
  (ref: comm. 2002-05-15 astrometryGap). This translation will be adjusted for by modifying the number of overscan collumns.
- as of 2002-05-18, the translation has been corrected for by software, adjusting the number of pre-scan column on each chip. Now, directly joining the 4 subimages will produce an image geometrically correct within 1 pixel in the central region (Y~2000). The geometrical error goes up to 2pix at the top and bottom of the gap.
CCD rotation: as of 2002-05-15, there is a small rotation of the slave CCD with respect to the master:

Delta X = 0.90 over 4000pix
Delta Y = 0.35 over 4000pix.

(ref: comm. 2002-05-15 astrometryGap) These values correspond to a rotation of 0.22 mrad. As this corresponds to a physical rotation of the CCD, it cannot be adjusted.

Optical axis / Field center / Flexures : In order to avoid that the main object falls in the inter-chip gap, the mosaic has been slightly shifted in the dewar. The actual position is measured by determining the center of rotation of the image while rotating the rotator (i.e. we assume that the optical axis is on the rotator axis, cf R.Wilson [4]). In order to estimate the instrumental flexures, this is done for 4 angles, computing the rotation from -5 to 5deg, 85 to 95, etc... (ref: comm. 2002-05-15, astrometryCenter and [3] for the find_center.prg procedure). The values below are given in the pixel system as of 2002-05-15 (i.e. before the master CCD shift by 2 pix, PSI 2002-05-16) - after 2002-05-16, the Y of the master should be increased by 2pix.

Table: Position of the center of rotation (and optical axis) and flexures

	Master Chip		Slave chip (left)
Rotator Angle on Sky	x	y	x	y
0	2318.05	2013.7	2344.9	2012.7
90	2319.6	2013.9	2345.5	2012.2
180	2313.2	2014.3	2340.9	2012.4
270	2319.5	2016.4	2345.8	2015.3

Figure: Field of View and orientation.
This image corresponds to a full 4x4k flat field. The grey area is the illuminated area.

Dome Flatfields

The following information was obtained using the 1x1 binning mode, with "Normal" read-out mode, slit width = 1". The exposure time given below are computed for a given expected peak level (EXPLEVEL) of 20 000 ADU. Halogen lamps were used. The Plot col. links postscript plots of cuts through these FF (H and V for horizontal and vertical cut respectively, taken at ~the center of the image), showing that the they are extremely good and flat over the available field of view.

Table: Imaging Dome FF conditions

Filter	Lamps (internal units)	Exposure Time (s)	Plots (gzipped ps)
Bb#605	2 x 128	11	H V
V#606	1 x 60	35	H V
R#608	1 x 40	33	H V
I#610	1 x 30	42	H V

Photometry and Throughputs

The following photometric solution was obtained on one single standard field with 4 stars, taken in poor seeing conditions; it obviously needs to be refined (ref: Comm.2002-05-11 stdPhot).

Table: Photometric solution. The left column refers to the standard magnitudes, the right-hand one to the instrumental magnitudes (obtained from the electron counts). The extinctions are the standard La Silla ones, Z is the airmass.

Filter	Equation
Bb=	bb+ 25.27+/-0.03 + ( 0.018+/-0.079)(B-V) -0.214Z
V=	v + 25.98+/-0.01 + (-0.009+/-0.022)(V-R) -0.125Z
R=	r + 26.21+/-0.02 + (-0.041+/-0.040)(V-R) -0.091Z
I=	i + 25.57+/-0.03 + (-0.024+/-0.082)(R-I) -0.051Z

Table: Count Rates, for a Mag=15 star, in electron/s, at airmass = 1

Filter	Counts
Bb	13439
V	25712
R	31185
I	17915

Low Resolution Spectroscopy (RILD)

For the orientation of the spectra, refer to the figure earlier on this page.

Wavelength ranges, pixel size, etc.

Table: Wavelength ranges and resolution for RILD Grisms.

Grism #	Wavelength range (nm)	Pixel size (nm)	Resolution *
1	385 - 1000	0.37	290
2	385 - 930	0.18	590
3	385 - 850	0.14	760
4	445 - 1000	0.17	830
5	380 - 670	0.083	1280
6	575 - 875	0.075	1700
7	385 - 1000	0.35	300

* Measured at 587.6 nm except grism #6 at 706 nm

With the new geometry of the CCD, Blue is down (small Y), Red is up (large Y).

Note that because of the larger size of the new CCD, the wavelength coverage is much larger than what it used to be. As a consequence, many grism now present a second order contamination. Use the table below for order separating filter selection.

Table: Order separating filters. (full list of filters available elsewhere )


Order-sorting filters
643	BG38 2mm	481.9	276.9	96	R2	ps dat
645	OG530 3mm	>530.0	lwp	95	R1	ps dat
646	RG715 3mm	>721.5	lwp	98	R3	ps dat
769	BG39	472.2	237.2	86	R3	ps dat

Dome Flat-Fields

The following information was obtained using the 1x1 binning mode, with "Normal" read-out mode, slit width = 1". The resulting exposure time is automatically computed by the REMD_spec_cal_Flats template, for a given expected peak level (EXPLEVEL) in ADU. The CCD saturates above 60 000 ADU. The plots of the FF are roughly calibrated in wavelentgh. A example of horizontal cut in one of the FF can be found here.

Grism	Expected Peak Level (ADU)	Exposure Time (s)	Plot
#1	40 000	6.0	ps gif
#2	40 000	5.9	ps gif
#3	40 000	8.1	ps gif
#4	40 000	9.3	ps gif
#5	40 000	15.1	ps gif
#6	40 000	18.1	ps gif
#7	40 000	6.5	ps gif

Wavelength Calibrations

Exposure times

The table below lists the updated exposure times for the new CCD. Note that they are similar to those used with the previous chip.

Table: Grism Wavelength Calibration Exposure Times

Grism	He	Ar
Grism #1	2	1
Grism #2	2	2
Grism #3	2	2
Grism #4	5	1
Grism #5 (with filter BG38#643)	3	300
Grism #6	6	2
Grism #7	2	1

Wavelength Atlas

To be used for line identification and order selection filters. The plot present the full extension of the CCD (i.e. the 4000 pixels)

Table: Wavelength Atlas

Grism#1	Grism#2	Grism#3	Grism#4	Grism#5	Grism#6	Grism#7
gif ps	gif ps	gif ps	gif ps	gif ps	gif ps	gif ps

Throughputs

The table below lists the throughputs of the Grisms, in electron/sec/nm for a 12th magnitude AO star at airmass 1. A more detailed version of this table is available as an ASCII file.

Table: Grism Throughputs, in electron/sec/nm, mag=12 at airm=1

Wavelength[nm]	Gr1 Gr1	Gr2 Gr2	Gr3 Gr3	Gr4 Gr4	Gr5 Gr5	Gr6 Gr6	Gr7
360	1	0	-	-	-	-	0
400	0	53	29	-	-	-	0
440	1	131	149	-	-	-	0
480	0	164	181	1	-	-	0
520	40	180	178	1	-	-	0
560	180	188	184	2	-	-	27
600	247	196	187	59	-	-	111
640	286	200	179	119	-	-	192
680	300	181	151	147	-	-	238
720	310	158	125	157	-	-	251
760	278	130	104	157	-	-	237
800	241	125	97	151	-	-	216
840	209	125	82	143	-	-	193
880	212	113	74	146	-	-	176
920	241	104	-	133	-	-	179
960	225	79	-	87	-	-	125
1000	174	-	-	42	-	-	78

Medium Resolution Spectroscopy (REMD-spec)

For the orientation of the spectra, refer to the figure earlier on this page.

Wavelength ranges, pixel sizes, resolutions, etc

Wavelength Atlas

The HeAr spectra corresponding at the "standard central wavelentghts" (defined in our calibration plan) are listd below. Of course, for scientific observations, any central wavelength can be selected.

Table: REMD-spec Wavelength Atlas

Grating	Exposure Time (s) He + Ar	Central Wavelentgh (NM)	Atlas
#6	15 + 300	490	ps gif
	0 + 300	550	ps gif
	1 + 300	610	ps gif
	6 + 15	670	ps gif
	6 + 10	730	ps gif
	0 + 3*	790	ps gif
	0 + 7*	850	ps gif
	0 + 5*	910	ps gif
	0 + 5*	950	ps gif
#7	10 + 150	500	ps gif
	1 + 60	630	ps gif
	9 + 2*	760	ps gif
	0 + 4	890	ps gif
#8	12 + 60	575	ps gif
	8 + 2*	825	ps gif
#13	3 + 2	700	ps gif

*Note: with Filter OG530#645

Dome Flat-Fields

Grating	Central Wavelength (nm)	Expected Peak Level (ADU)	Lamps (W)	Exposure Time (s)	Plot
#6	490	20 000	5300	32	ps gif
	550	20 000	5300	15	ps gif
	610	20 000	5300	11	ps gif
	670	20 000	5300	10	ps gif
	730	20 000	5300	10	ps
	790	20 000	5300	10	ps gif
	850	20 000	5300	10	ps gif
	910	20 000	5300	11	ps gif
	950	20 000	5300	13	ps gif
#7	500	45 000	8400	14	ps gif
	630	45 000	8400	7	ps gif
	760	45 000	6400	9	ps gif
	890	45 000	6400	9	ps
#8	575	20 000	1300	14	ps
	825	20 000	1300	7	ps gif
#13	700	20 000	1300	7	ps gif

Throughputs

Not available yet (still raining...).

High Resolution Spectroscopy (REMD-ech)

This mode is described in more details on the REMD-ech page.

Orientation

For the orientation of the spectra, refer to the figure earlier on this page.

Dome Flat-Fields

The following information was obtained using the 1x1 binning mode, with "Normal" read-out mode. The resulting exposure time is automatically computed by the REMD_ech_cal_Flats template, for a given expected peak level (EXPLEVEL) in ADU. We provide in the table below an image of the flat, and the corresponding FITS file as well, to allow users to use it.

Grating

Grism

Slit Width

Expected Peak Level
(ADU)

Lamps (W)

Exposure Time

Plot

#9

#3

1 x 10 ''

30 000

8400

32

gif fits

#4

1 x 20 ''

30 000

8400

14

gif fits

#10

#3

1 x 3 ''

30 000

8400

227

gif fits

#4

1 x 5 ''

30 000

8400

87

gif fits

#5

1 x 6 ''

30 000

8400

200

gif fits

#6

1 x 15 ''

30 000

8400

112

gif fits

#14

#3

1 x 3 ''

30 000

8400

176

gif fits

#4

1 x 5 ''

30 000

8400

71

gif fits

#5

1 x 5 ''

30 000

8400

not available yet

#6

1 x 15 ''

30 000

8400

not available yet

Wavelength Calibrations

The following table list the recommended exposure times for a 2x2 bin CCD and links the "finding charts" for the orders and reference lines. It also links the FITS files countaining the flatfield and ThAr lamps. Potential observers are suggested to download these frames to experiment with the effect of the inter-chip gap on their data reduction software. Feedback is most welcome. Note that the gzipped FITS frames are big.

Table: Echelle wavelength calibrations

Grating	Cross Dispersor Grism	Exp.Time [sec], Th lamp alone, Ar is included	Atlas	FITS
#9	Grs#3	600	gif	ThAr
	Grs#4	180	gif	ThAr
#10	Grs#3	1200	not available yet	ThAr
	Grs#4	600	not available yet	ThAr
	Grs#5	600	gif	ThAr
	Grs#6	150	gif	ThAr
#14	Grs#3	900	gif	ThAr
	Grs#4	900	gif	ThAr
	Grs#5	900	gif	ThAr
	Grs#6	900	gif	ThAr

FITS file, hints and tips

FITS

The FITS frames produced by the new EMMI-Red CCD are written as "multiple extention FITS file". In the modes offered, the images come in 4 extensions corresponding to the 2x2 amplifiers.A small MIDAS procedure is available to read-in new EMMI red frames and paste the pieces together. ]
Header: most of the generic keywords are in the first FITS extension, which contains no data. The following 4 extensions (which contain one image each) list the keywords related to each chip.
The read-out speed is in HIERARCH_ESO_DET_READ_CLOCK, where it is listed in kps (625=fast, 225=normal, 100=slow). The read speed is listed are normal in all modes.

Observing Templates

The current Instrument Package (EMMI-IP-20020212) is still valid. However, it must be noted that

while windowing can still be defined, it is ignored by the instrument.While other combinations are valid in P2PP, the only binning allowed are 1x1 and 2x2.
As of today (2002-05-12), only 1x1 is offered for science exposure.The spectral dispersion used to be along x, it is now along y (does not matter at the level of OB definition).

Templates wer fully commissioned. A new internal IP was released. It is not made a public release, as the current official one is compatible with the new detector.

DIMD mode is not offered yet. MOS templates have been commissioned "on dome". XMos package is being modified.

Final word: "Dans le sirop de poire, les souris coulent". Don't ask.

Acceptance

ORIGINAL REQUIREMENT AS IN [2]	COMMENTS	STATUS
QE as table in [2]:	verified in the lab:	[OK]
Chip geometry [2]	distance to flange and planeity measured in lab: OK. Gap and rotation: OK.	[OK]
Binning modes required: 1x1 and 2x2:	all certified, except 1x1/625kps, which did present twice during the commissioning an abrupt drop of bias on 3 chanels (BCD).	[OK]/[PENDING]
Read-out modes required: "Slow" at ~100kps and "Fast" at ~300kps	Modes provided are better than specs (100, 225, 625kps)	[OK]
RON<4e at 100kps	3.5e at 100kps, ~8 at 225, i.e. within spec. However, a small pick up noise is detected, and will be eliminated.	[OK]
Windowing in one chip	Considering the read-out times, hardware windowing requirement was dropped, and replaced by software windowing, pending FIERA sofware upgrade for software windowing.	[OK]/[PENDING]
Dark current < 2e/h	< 1e-/h/pix average, few pixels ~5e-/h/pix	[OK]
Linearity deviation < 0.5% up to 120000e-	<0.5% in all modes up to 65kadu	[OK]
Persistency: saturation leaves < 20e remnant in 30min exp	no remnance detected	[OK]
Cosmetics: <5 bad columns, no major defect	2 bad cols, very few bad pixels, no defect at all	[OK]
Observing templates updated	tested OK, ISF updated, backward compatible with pre-upgrade instrument package. New internal instrument package released	[OK]
Set-up templates updated	tested OK.	[OK]
Initial calibration plan: Imaging	astrometry and photometry performed. In agreement with expectations	[OK]
Initial calibration plan: Spectro	Wavelength atlas and flat field in all modes acquired. Spectroscopic throughput in 5/7 grisms, 0/4 grating, 2/10 echelle combinations in agreement with expectation. Others pending	[OK]/[PENDING]
xMOS package update	data acquired and processed. Implementation pending, scheduled for May 24.	[PENDING]

PROJECT		[OK]

Grating	Grism	Slit Width	Expected Peak Level (ADU)	Lamps (W)	Exposure Time	Plot
#9	#3	1 x 10 ''	30 000	8400	32	gif fits
	#4	1 x 20 ''	30 000	8400	14	gif fits
#10	#3	1 x 3 ''	30 000	8400	227	gif fits
	#4	1 x 5 ''	30 000	8400	87	gif fits
	#5	1 x 6 ''	30 000	8400	200	gif fits
	#6	1 x 15 ''	30 000	8400	112	gif fits
#14	#3	1 x 3 ''	30 000	8400	176	gif fits
	#4	1 x 5 ''	30 000	8400	71	gif fits
	#5	1 x 5 ''	30 000	8400	not available yet
	#6	1 x 15 ''	30 000	8400	not available yet

EUROPEAN SOUTHERN OBSERVATORY

La Silla Science Operations: NTT

EMMI

New RED CCD Commissioning report and notes for the observer

Table of Content

Commissioning

Introduction

Purpose and scope

Document

CCD, bias and dark

Hardware and Geometry

Read-Out Modes

Dark current

Linearity

Read-Out Times

Quantum Efficiency

Imaging

Astrometry

Dome Flatfields

Photometry and Throughputs

Low Resolution Spectroscopy (RILD)

Wavelength ranges, pixel size, etc.

Dome Flat-Fields

Wavelength Calibrations

Exposure times

Wavelength Atlas

Throughputs

Medium Resolution Spectroscopy (REMD-spec)

Wavelength ranges, pixel sizes, resolutions, etc

Wavelength Atlas

Dome Flat-Fields

Throughputs

High Resolution Spectroscopy (REMD-ech)

Orientation

Dome Flat-Fields

Wavelength Calibrations

FITS file, hints and tips

FITS

Observing Templates

Acceptance

New RED CCD
Commissioning report and
notes for the observer