NACO Science Verification
Programs at Yepun/UT4

• NACO/WFPC2 deep field Raw Data Available
• NACO Observations of a Deep NICMOS field in the Bulge Raw Data Available
• Spatially Resolved Spectroscopy of Sy1 and Sy2 Galaxies
• Spatially Resolved Central Stellar Velocity Dispersion in Ellipticals (Not executed)
• QSO Environments (Not executed)
• Imaging of Multiple-image Gravitational Lens systems

• Imaging and Spectroscopy of the the Pluto-Charon system (Not executed)

• Planetary/Protoplanetary candidates
• Circumstellar envelopes (Not executed)
• NACO Observations of Mira Raw Data Available
• Star forming regions
• Galactic Center Raw Data Available

A Summary of SV Observations is now available

Details can be found in the Night Logs:
[2002-08-16+17] [2002-08-17+18] [2002-08-18+19] [2002-08-19+20] [2002-08-20+21] [2002-08-21+22] [2002-08-22+23] [2002-08-23+24] [2002-08-24+25] [2002-08-25+26] [2002-08-26+27] [2002-08-27+28] [2002-08-28+29] [2002-08-29+30]

Useful Links/Documents

Preparing OBs

NACO SV Meetings

• Mar 08, 2002 Agenda
• May 14, 2002 Agenda - Wolfgang's PPT presentation
• July 5, 2002 Agenda
• July 5, 2002 Action Items
• NACO SV Team

NACO/WFPC2 Deep Field [Get RAW DATA]

 

Target:	Casertano field (F606W, 80x80"): RA = 22:53:37.3, DEC = -14:27:40
Mode:	Imaging in Ks & J band
ExpTime:	2hr per filter + overhead = 5hr
Conditions:	photometric, seeing <0.7"
Objective:	Test performance of NACO deep imaging on non-point sources by comparing it with an HST-WFPC2 deep field.
Coordinator:	M.Lehnert, A.Moorwood, P.Rosati

 

NACO Observations of a Deep NICMOS field in the Bulge   [Summary] [Get RAW DATA]

 

Target:	Bulge field: RA = 18:11:04.5,  DEC = -31:45:49 [NIC2 image, 22x22", J-band ] [I-band WFI image]
Mode:	Imaging in H, Ks & J band
ExpTime:	Exp Times (hours, incl.overheads): 6.5 (J), 1.3 (H), 4.8 (K) [Total = 12.8]
Conditions:	photometric, seeing <~0.8"
Objective:	Reduced NICMOS imaging will be made public to allow a direct comparison of NACO and NICMOS imaging in J,H bands (photometric accuracy, depth). By complementing NICMOS data with NACO K-band data one will be able to further improve the determination of the IMF of the bulge stars. A catalog and a FITS image in H+J band of the NICMOS field is also available for such comparison (courtesy of M.Zoccali).
Coordinator:	A.Renzini, M.Zoccali

 

Spatially Resolved Spectroscopy of Seyfert Galaxies   [Summary]

 

Targets:	NGC 1386: (Sy2, z=742 km/s, K=10.7 in 2" ap) RA = RA=03 36 45.42,   DEC = -35 59 56.7 [DSS 5x5'] [Simbad Info] NGC 1097: (Sy1, z=1285 km/s, K=10.6 in 2" ap) RA = 2:46:19.2,  DEC = -30:16:29 [DSS 5x5'] [Simbad Info] NGC 7582: (Sy2, z=1545 km/s, K=9.4 in 2" ap)RA = 23:18:23.3,  DEC = -42:22:16 [DSS 5x5'] [Simbad Info]
Mode:	N1386, N1097: imaging in K,H,L,J bands (see priority) and spectroscopy (in H,K,L). N7582: spectroscopy only to complement GTO program. Target priority: N7582, N1097, N1386.
ExpTime:	3 hrs for imaging (2 targets, 4 bands); 2 hrs total for spectroscopy (2 slit positions)
Conditions:	clear, seeing <1"
Objective:	Spatially resolved spectroscopy of the core of Seyfert galaxies with the aim of probing the transition between stellar continuum and AGN powered inner regions. Search for broadline regions in Sy2 (predicted by unified models).
Coordinators:	Y.Clenet, V.Ivanov, L.Tacconi-Garman

 

Spatially Resolved Central Stellar Velocity Dispersion in Ellipticals

 

Targets:	TBD, from (images of 6 targets): Name RA Dec V (or H) Sep (") -------------------------------------------------------- IC4451(*) 14 34 37.2 -36 17 07 10.50 28.9 NGC5838 15 05 26.2 02 05 58 14.84 --- IC4742(*) 18 41 53.2 -63 51 44 9.74 39.2 ESO184-G005(*) 19 03 39.5 -53 56 10 10.01 33.3 NGC7484(*) 23 07 04.5 -36 16 28 9.91 49.3 NGC7626 23 20 42.3 08 13 02 13.24 --- Those with (*) have nearby stars of mag V at separation indicated. Others have central H-band central surface brightnesses quoted.
Mode:	spectroscopy in H and K, imaging in JHKs bands
ExpTime:	TBD
Conditions:	photometric/clear, seeing <~0.5"
Objective:	To test the NACO performance on cuspy ellipticals versus stars at relatively large distances, to obtain deep NIR spatially resolved velocity dispersion measurements to probe E formation scenarios, to search for counter-rotating core(s), to determine spatially resolved M/L
Coordinators:	L.Tacconi-Garman

 

QSO Environments

 

Targets:	TBD, from: Name RA (J2000) DEC V z ------------------------------------------------------- Q_2200-1816 22 03 11.6 -18 01 42 15.50 1.16 HE_0353-3919 03 55 09.9 -39 10 27 15.60 1.001 HE_0515-4414 05 17 07.6 -44 10 56 14.90 1.713
Mode:	K band imaging
ExpTime:	One target only, 2.5 hrs (including overhead)
Conditions:	clear, seeing <0.6"
Objective:	Study of the closest environment of QSOs
Coordinators:	Y.Clenet, A-M. Lagrange

 

Imaging and Spectroscopy of the Pluto-Charon system

 
Imaging in Ks band + spectroscopy

Target:	Pluto: RA = 17:04, V=14, ang_size=0.11"; (Charon: V~=15.5)
Mode:	Attempt observations of occultation of a GSC star by Pluto on July 19-20. Spectrosopy in K and L bands.
ExpTime:	Obtaine 5-10 images/sec during the ~3 minutes of the occultation (0.1 sec individual exposures). Spectroscopic program requires a total of 3 hours. Total time needed to complete Pluto programme: 6 hours
Conditions:	clear, seeing <1.1"
Objective:	The pluto stellar occulation of July 20th, 2002 offers a rare and unique oppurtunity to probe the chemical composition and physical parameters of the Pluto atmosphere (detailed and updated information on this event can be found at this web site, maintened by B.Sicardy). See also these detailed notes by A-M. Lagrange. NACO spectroscopy of the Pluto-Charon system in the 1.8 to 3.6 micron range will give access to important molecular absorption bands to probe composition differences between Pluto and Charon.
Coordinator:	A-M. Lagrange, W.Brandner

 

Planetary/Protoplanetary candidates  [Summary]

 

Targets:	HD163296 RA(2000)=17:56:21.28, DEC=-21:57:21.9 - A1 V=6.9
Mode:	Coronography in H and/or K bands. Polarimetry (Wollaston prism) in H and Ks bands
ExpTime:	Coronography: 3 hrs total (one band only, K or H depending on atmospheric conditions) Polarimetry: 1.5 hrs (incl. overhead, one band)
Conditions:	clear, seeing <0.8"
Objective:	Observations of proto-planetary candidates with the aim of detecting circumstellar (CS) material around young stars, measuring their sizes and asymmetries. HST observations have revealed CS disks for both HR4796 (with NICMOS, Schneider et al. 1999), and HD 163296 (with STIS, Grady et al. 2000). NACO coronographic observations will allow the CS to be imaged with a spatial resolution better than HST. NACO polarimetric observations will allow the polarized light from the disk to be separated from the unpolarized light from the star.
Coordinator:	N.Huelamo, A-M. Lagrange, W.Brandner, N.Ageorge

 

Circumstellar Envelopes

 

Targets:	IRAS 16594-4656: (16:03:09.7 -47:00:28) I=12.0, K=8.2 IRAS 17245-3951: (17:28:04.8 -39:53:44) I=13.2, K=9.7 IRAS 20136+1309: (20:16:00.1 +13:18:55) I=12.0, K=8.0 IRAS 17106-3046: (17:13:51.7 -30:49:40) J=9.95; H=8.94; K=8.34 IRAS 17150-3224: (17:18:20.1 -32:27:23) J=11.1; H=10.22; K=9.45 IRAS 18184-1302: (18:21:15.9 -13:01:27) B=13.9 - Sp.Typ. = Be
Mode:	Imaging in J,H,K,L bands + Br gamma Polarimetric imaging in J,H,K
ExpTime:	Two targets only to be selected from list above (sorted by priority) Typically, 1 hour/filter. Specifically, for IRAS 17150-3224 & IRAS 18184-1302: 24min in J, 16 min in H & 12 min in K on source -> 2*52min+overheads=3 hours. Total time needed for two targets: 6 hrs
Conditions:	clear, seeing <0.8"
Objective:	Observations of bipolar or multi-polar post-AGB circumstellar Envelopes to constrain physical models of envelope ejection [more info].
Coordinator:	A-M. Lagrange, N.Ageorges

 

Star forming region [README]

 

Targets:	g45.45 (center, J2000) 19:14:21.3 +11:09:13.5
Mode:	J, H, K, BrG
ExpTime:	Total integration = 56 min+overhead = 2 hrs
Conditions:	clear, seeing <1"
Objective:	Follow-up observations (deeper and higher angular resolution) of a ultracompact HII region (observerd by AO systems ADONIS and Gemini North; at least 8 O-stars identified inside, large amounts of hot dust + one obscured (in K) source to the north).
Coordinator:	M.Feldt

 

NACO Observations of Mira [README] [Get RAW DATA]

 

Targets:	Mira (center, J2000) 02:19:20.79 -02:58:39.50 (J=-1.0, K=-2.4)
Mode:	Narrow band filters
ExpTime:	As short as possible
Conditions:	clear, seeing <1"
Objective:	This programme aims at resolving Mira in and out of molecular lines/bands by means of narrow-band imaging.
Coordinator:	W.Brandner, A.Richichi

 

Galactic Center [Summary] [Get RAW DATA]   See also data for this programme obtained during commissioning

 

Targets:	Galactic Center (J2000) 17:45:40.0 -29:00:35
Mode:	H,K, and L' bands
ExpTime:	Total integration = 1.5 hr + overhead
Conditions:	clear
Objective:	An imaging program to obtain deep H,K, and L' exposures in the Galactic Center field.
Coordinator:	M.Lehnert

 

Imaging of Multiple-image Gravitational Lens systems

 

Targets:	PKS1830-211 (RA, Dec, J2000) [finding chart (Courbin et al. 2002)]
Mode:	J or K
ExpTime:	Total integration = TBD
Conditions:	clear, seeing <0.6"
Objective:	High resolution imaging of a gravitationally lensed radio source (at z=2.507) to improve the lesing model. HST obsevations (with WFPC2 and NICOMOS) and AO imaging with Gemini North already exist.
Coordinator:	L.Tacconi-Garman

 

Send comments to <arenzini@eso.org> Last update: July 15, 2002