GEMINI OBSERVATORY
observing time request (HTML summary)

Semester: 2004BPartner reference:
Not Available
PI time requested:
60.0 hours
Gemini reference:
Not Available
Partner ranking:
Not Available
PI minimum time requested:
8.0 nights
Instruments(s):
NIRI+Altair
NTAC recommended time:
0.0 nights
PI future time requested:
8.0 nights
Observing mode: classicalNTAC minimum recommended:
0.0 nights
PI total from all partners: 0.0 nights
(joint proposals)
Time awarded:
Not Available
Proposal submitted to: Canada


Title:Merging, Morphology and Mass Build-up in the CFHTLS Deep Fields
Principal Investigator:Stephen Gwyn
PI institution:University of Victoria, Department of Physics and Astronomy,PO Box 3055,Victoria,BC,V8W 3P6,Canada
PI status:PhD/Doctorate
PI phone / fax / e-mail:250-721-8656 / 250-721-8656 / gwyn@uvastro.phys.uvic.ca
Principal Contact:Stephen Gwyn
PC institution:University of Victoria
PC phone / fax / e-mail:250-721-8656 / 250-721-8656 / gwyn@uvastro.phys.uvic.ca
Co-investigators:Ray Carlberg: University of Toronto, carlberg@astro.utoronto.ca
Dave Patton: Trent University, dpatton@trentu.ca
Tim Davidge: Herzberg Institute of Astrophysics, Tim.Davidge@nrc-cnrc.gc.ca
Luc Simard: Herzberg Institute of Astrophysics, Luc.Simard@nrc-cnrc.gc.ca
Carrie Bridge: University of Toronto, bridge@astro.utoronto.ca
Cathy Perrett: University of Toronto, perrett@astro.utoronto.ca

Abstract: We propose a deep, targeted imaging survey down to K_AB=25 with Altair+NIRI. Twenty fields near bright guide stars will be selected in each of the CFHT Legacy Deep fields to study three aspects of galaxy evolution:

- We will measure the galaxy merger rate at high redshift by determining the abundance and morphologies of close galaxy pairs

- High resolution K-band images will trace the evolution with redshift of the morphology of the quiescent stellar populations

- Using K-band luminosity as a tracer of stellar mass, we will be able to follow the build-up of the mass of stars in galaxies from z~3 to the present.

In a subsequent proposal we will undertake AO spectroscopy using Altair+NIFS of a subset of the objects to create a redshift survey between 2 and 3 magnitudes deeper than any other K selected sample.


Science Justification

Background:

The hierarchical clustering model of galaxy formation, particularly within the Cold Dark Matter theory for structure formation, makes many quantitative predictions about the evolution of galaxy masses and galaxy clustering properties. To a significant degree these theories (particularly the semi-analytic approach) are normalized to low redshift data. Tests of the models are then most powerful at increasingly high redshifts. There is widespread agreement that the "feedback processes" are difficult to handle and need observational guidance.

Hierarchical models indicate that galaxy evolution works bottom-up: small structures form first. Recent observations suggest that, although the dark matter may assemble in this manner, stars form in large galaxies first. There is increasing evidence that the mass assembly of large galaxies takes place well beyond z=1. Recent work by the Gemini Deep Deep Survey (GDDS, Glazebrook et al. 2004) shows that most of the stellar mass in bright galaxies has already been assembled by z=1. Im et al. (2002) show that large ellipticals were already mostly in place at z=1, and that they were already old at this epoch.

While these are very important results, and arguably in strong disagreement with the hierarchal model, these studies do not probe far enough out in redshift to find the epoch of mass assembly (z>2), nor do they go very far down the luminosity function of galaxies at z>1.5. In order to study the less massive galaxies which are more representative of the galaxy population as a whole, it is necessary to go deeper.

We propose a deep, targeted imaging survey down to K_AB=25. This is 2-3 magnitudes deeper than the GDDS and the Las Campanas InfraRed Survey. Using the adaptive optics system of ALTAIR+NIRI on Gemini, we will get 0.08" FWHM images of galaxies, three times better in resolution than the space-based NICMOS images from HST and covering a much larger area. The superb resolution of these AO images will enable us to observe galaxies as faint as K_AB=25 in one hour integrations. At these magnitudes, most of the objects are at z>1 (See Figure 1) and there is a significant population out to z=3-4.

The targets will be selected in the CFHTLS Deep fields. These fields provide u'g'r'i'z' data down to about 26 AB magnitude (at this point in time) over four square degrees of sky. This ongoing survey will extend another magnitude deeper when it is completed, approaching the depth of the HDF. The multi-colour CFHTLS data already yield excellent photometric redshifts (Gwyn et al. 2004) which will be further refined with K data. The large size of the fields (1 degree = 30 Mpc at z=1) means that we can sample a range of local density environments from isolated field galaxies to galaxy clusters (each square degree of the CFHTLS images contains on the order of 10 galaxy clusters). Density maps of the fields are being prepared using photometric redshifts to split the fields into redshift slices and measuring the local surface density of galaxies in co-moving volumes of one Mpc in projected radius (Nuyten et al. 2004). In addition, one of the fields (the CFHTLS-D2) is embedded in the HST-ACS COSMOS public field. These high-resolution space-based data will provide morphologies in the optical (rest frame UV) which will complement the K band (rest frame optical) data we will obtain.

Given our need for AO, the main driver of field selection must be the R(Vega)<13.5 guide stars in the square degree of each CFHTLS Deep Field. Each 22x22 arcsecond field covers about 0.1 square arcminutes, after allowances are made for the area swamped by the guide star itself. Picking subfields around the randomly placed guide stars means that we are sparsely sampling the area. This means that we take advantage of the large size of the CFHTLS fields to look at un-correlated parts of the universe and partially avoid the problems with cosmic variance.

The observations in the current proposal will address three aspects of galaxy evolution: Merging, morphology and mass-buildup.

-Merger rates:

One relatively robust prediction of hierarchical models is the evolution of the two-point correlation function, which at the small scale end is simply the close galaxy pairs. These pairs are the precursors to merging events which play a central role in determining the evolution of galaxy masses, star formation, and galaxy morphology. Close pairs have been used to estimate the galaxy merger rate and its evolution at low redshift (e.g., Patton et al 2000,2002, Le Fevre et al. 2000; Bundy et al. 2004). However, these studies indicate that the epoch of peak merging occurred at higher redshifts (z > 1).

One of the central goals of this proposal is to make comparable measurements at high redshift, using deep imaging at similar rest-frame wavelengths (optical). Extrapolation from various lower redshift samples yields a conservative prediction of 10-20% of galaxies residing in close pairs at z > 1. This is consistent with estimates of the fraction of high redshift galaxies that have disturbed morphologies (Conselice et al. 2003).

To make a confident measure of the merger rate beyond redshift one, we need to find 80 physical pairs in a deep K sample. Given that we need to draw the pair sample from a sky area in which 160 paired galaxies are seen, this requires a parent sample of 800 random field galaxies. The NICMOS/HDF studies found that there are about 50 galaxies per square arcminute at m_AB(K)=25 mag (Thompson et al. 1999). Therefore we need a sample that covers about 16 square arcminutes (rather than the 2/3 square arcminute of the NICMOS sample). Given that one NIRI f/32 image covers about 0.1 square arcminutes, this implies 160 guide stars are needed. Of these 160 guide star fields, about half will contain one or more close physical pairs. By pre-selecting 80 fields with high probability pairs (see Technical Justification), we should observe close to 80 physical pairs, of which approximately half (Patton et al 2000) are likely to be merging, as evidenced by their disturbed morphologies. This sample of about 40 merging galaxy pairs will be compared with the parent sample of 800 galaxies to yield a clear estimate of the high redshift merger rate.

-Morphology studies:

In addition to being able to detect disturbed morphologies in the interacting galaxies, we will also measure the morphologies of the other 400 or so normal galaxies in the observed fields.

The era before z=1 studied in this survey is an interesting one for galaxy morphology. At z>2 most galaxies show very disturbed morphologies while at z<1 most of the standard Hubble "tuning fork" sequence of morphologies is largely in place. There are a number of studies (eg. Abraham et al. 1996, Im et al 2002) which use quantitative morphology methods to study this evolution. All of these studies used images in optical bands. At z>1 even fairly red optical bands show the galaxy in the rest frame UV, where the transitory effects of starbursts dominate the morphology. By switching to the infrared we can study the underlying structure of galaxies.

The quantitative morphology software package, GIM2D (Simard et al. 2002), decomposes the image of a galaxy into its components (a bulge and a disk),computes the relative contributions of each component to the total light of the galaxy and the properties of each component (e.g disk scale length). We would use this software to trace the change of various morphological properties with redshift and environment. For example, we will be able to follow the growth of disk scale length as a function of time. Another project will be to see if the appearance of bulge dominated systems occurs earlier in higher density environments.

Selecting the sample in K is uniquely suited to finding red, dust-enshrouded disk galaxies. A few have been found in a cluster at z=1.27 (Wu et al 2003). Finding some of these objects would help bridge the gap between the normal star-forming galaxies found in the optical and the extremely obscured, dusty objects that show up as SCUBA sources.

As mentioned earlier, the CFHTLS-D2 field will have extensive HST optical imaging. One can combine the two data sets by generating a model for the morphology of a given galaxy in the K band and subtracting this model from the HST image of the same galaxy. The resulting image gives a picture of the location of star formation in that galaxy.

-Mass-build up:

The UV and blue light from galaxies is dominated by short-lived, high mass stars and is therefore a poor indicator of stellar mass. The red/IR light from galaxies comes from longer-lived objects is therefore a much better tracer of mass. Although there is a direct correlation between K-band luminosity and stellar mass, the fitting methods used by Glazebrook et al. (2004) and Dickinson et al. (2003) are a better approach. In these methods, spectral energy distributions (SED) are modelled with a variety of star formation histories. The actual SED of a galaxy is determined from its colours and compared to the synthetic SEDs to determine its star formation history and therefore its current stellar mass. This fitting process has been shown to not be degenerate with photometric redshift. However if there are no bands covering the red end of the SED, it cannot put strong constraints on the stellar mass.

Having determined accurate mass measurement for these objects a number of studies will be possible. The most obvious of these is to observe the evolution of the mass function over time. The 400 galaxies that will be surveyed will allow us to split the sample into photometric redshift bins. If the naive interpretation of the hierarchal model is correct, then high redshift bins will be bottom heavy with respect to the low redshift bins. If the top down model is correct, the high redshift mass function will have a deficit of low mass objects. In order to be able to make definitive statements about the low-mass end of the mass function, it is absolutely vital to have deep K-band images; the K_AB=25 observations we propose extend 4 magnitudes below the K-band equivalent of L_* at z=1 and 2 mags below K* at z=3.

Further, the large size of this sample allows us study in which kind of objects the stellar mass is building up by splitting the sample into subsamples; red/quiescent vs. blue/star-bursts for example, or bulge-dominated galaxies vs. disks (as determined using the quantitative morphology method described above).

Finally, adding deep spectroscopy to the imaging provides a much richer dataset, with various spectral indicators of star formation (emission lines) and some indication of metallicity through line strength. In a subsequent proposal we will undertake AO spectroscopy using Altair+NIFS for a subset of the objects to create a redshift survey between 2 and 3 magnitudes deeper than any other K selected sample.

Attachments:

NameSourceType
Figure1nz_21_24_255.gifGIF
RefencesMMMrefs.txtTEXT

Technical Justification

In order to achieve the primary scientific objectives of this proposal, we need to observe a total of 400 galaxies. With 0.1 square arcminutes per NIRI field and 50 galaxies per square arcminute, we need to observe 80 NIRI fields. We plan to observe 20 NIRI fields in each of the four CFHTLS Deep fields. We will observe two Deep fields this semester (the D4 at 22hrs and the D1 at 2hrs) and two the next. Although we can withstand a reduction in the total sample of about a third (e.g. bad weather), reducing the number of observations by a half would severely compromise the statistical robustness of the studies proposed here.

To generate a well-defined set of targets for each CFHTLS field, we have picked the 40 faintest stars brighter than R_AB=14. As described in the Scientific Justification, roughly half of these fields are expected to contain a close physical galaxy pair. In order to maximize our chances of having these pairs land in our 20 guide star fields, each field has been examined for high probability pairs, using deep CFHTLS I-band images. The pairs which are most likely to be physically associated and likely to merge are those with projected separations less than about 20/h kpc, though additional merging pairs are certain to be found at larger separations as well (Patton et al. 2000). In converting this to an angular separation criterion, we take advantage of the fact that the angular diameter-distance relationship peaks at a redshift of about 1.5. Therefore, all angular pairs with separations less than 3.4 arcseconds must have projected physical separations of at most 20/h kpc, regardless of redshift (assuming that both galaxies lie at the same redshift).

Of the 40 guide star fields examined for each deep field, an average of 5 field galaxies were detected in the AO search area. This is consistent with the number of galaxies brighter than i' = 25.5 seen elsewhere in the images, and is in line with the expected counts brighter than K_AB=25. Overall, approximately 40% of these field galaxies are found in close angular pairs (< 3.4 arcsec), with many more being found in pairs closer than 50/h kpc projected separation. Using the observed counts of field and paired galaxies in these guide star fields, an objective algorithm was used to select the 20 best fields in each deep field. The resulting list of targets is given in the Observation Details. These fields contain an average of 7 field galaxies each, of which half are in close angular pairs.

Current tests indicate that the ground based data are useful to about 5" of the selected guide star. With a total field area of 22.4 arcsec squared the small circle lost in the centre leaves most of the area, for an average of about 0.1 square arcminutes per guide star. Existing Altair data show that one can do good photometry to within 3" of the guide star, so this will not set the limit. Figure 1 shows the typical geometry of a NIRI field.

We are requesting one hour total integration times. Calculations with the ITC indicate that this should be sufficient with AO guiding to reach K_AB=25 (K_Vega=23.2) with 20% photometry. Because the counts are quite shallow, about log_10(N) = 0.15 m_AB(K) + const (Thompson et al, 1999) there is a clear natural depth of exposure. Exposure times of much less than one hour lower efficiency as the setup time costs rise. Increasing the exposure time to 8 hours would increase the depth; the corresponding rise in the number of objects per unit area would be only about 50%. Since it would be possible to observe 5-6 fields in the same 8 hours, the total number of observable objects would decrease by a similar factor.

The observations will be photometrically calibrated using the guide stars themselves, which are all 2MASS sources.

For 20 targets with 30 minutes of setup time we request a total of 30 hours of CLASSICALLY scheduled Gemini time per CFHTLS Deep field. We are eager to learn as much as possible about the instrument by doing the observations ourselves. To allow for weather uncertainty we request 4 nights. Davidge will be the lead observer. He has considerable experience with ALTAIR already so there should be no "learning curve cost" at the telescope. This being said, if the TAC feels that we would be better served by switching to queue mode, we have no objections.

We are requesting the NIRI f/32 camera. Switching to the f/14 camera would increase the area surveyed and therefore decrease the total amount of telescope time required. However much of the area thus surveyed would be outside the isoplanatic patch. The loss in image quality would greatly hamper the ability the ability to discern disturbed morphologies in the interacting pairs. Further, in order to measure quantitative morphologies, GIM2D needs a well behaved PSF. The Strehl ratio decreases steadily with radius, but there is also a point beyond which the PSF can no longer be accurately described as elliptical but degenerates into a multi-lobed shape, making the computation of quantitative morphologies extremely difficult.

Because this project is closely related to two other public projects (CFHTLS and COSMOS), and because it will take a substantial amount of telescope time, we will release stacked images and catalogs to the CFHTLS community within six months of acquiring the last image.

Attachments:

NameSourceType
Figure 1pair.example.gifGIF
ReferencesMMMtechrefs.txtTEXT

Observation Details

ObservationRADecBrightnessTotal Time
(including overheads)
D4-MMM-122:14:46.504-17:15:53.054K_AB=251.5 hours
     S321132065 (oiwfs)22:14:46.53-17:15:53.1112.34 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-222:17:20.859-17:36:56.304K_AB=251.5 hours
     S3211120282 (oiwfs)22:17:20.858-17:36:56.4512.63 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-322:13:36.988-18:06:26.912K_AB=251.5 hours
     S3211320298 (oiwfs)22:13:36.997-18:06:26.8412.59 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-422:16:21.260-18:08:05.058K_AB=251.5 hours
     S321101028 (oiwfs)22:16:21.271-18:08:04.6712.86 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-522:14:40.487-17:51:18.750K_AB=251.5 hours
     S3211320217 (oiwfs)22:14:40.503-17:51:18.8212.72 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-622:16:27.764-17:49:20.707K_AB=251.5 hours
     S3211320204 (oiwfs)22:16:27.769-17:49:21.6512.82 Fmag separation 0.02
     observing conditions: Global Defaultresources:
D4-MMM-722:14:01.185-17:35:25.833K_AB=251.5 hours
     S3211320149 (oiwfs)22:14:01.218-17:35:25.6412.50 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-822:15:37.219-18:09:00.658K_AB=251.5 hours
     S321101034 (oiwfs)22:15:37.215-18:09:01.0712.90 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-922:15:11.656-17:14:45.896K_AB=251.5 hours
     S321132062 (oiwfs)22:15:11.673-17:14:45.6812.66 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1022:13:35.384-17:42:26.155K_AB=251.5 hours
     S3211320175 (oiwfs)22:13:35.392-17:42:25.8713.05 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1122:15:02.994-17:54:25.632K_AB=251.5 hours
     S3211320237 (oiwfs)22:15:02.995-17:54:25.7313.15 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-1222:14:00.233-17:53:13.122K_AB=251.5 hours
     S3211320231 (oiwfs)22:14:00.199-17:53:13.212.81 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1322:16:20.402-17:48:24.818K_AB=251.5 hours
     S3211320201 (oiwfs)22:16:20.407-17:48:25.2313.32 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1422:16:43.336-17:51:32.656K_AB=251.5 hours
     S3211320218 (oiwfs)22:16:43.339-17:51:33.0213.21 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1522:14:02.395-17:27:50.104K_AB=251.5 hours
     S321132086 (oiwfs)22:14:02.384-17:27:50.2713.35 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-1622:15:25.377-17:38:43.030K_AB=251.5 hours
     S3211320160 (oiwfs)22:15:25.38-17:38:43.1813.27 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-1722:13:35.857-17:14:32.934K_AB=251.5 hours
     S321132061 (oiwfs)22:13:35.861-17:14:32.713.16 Fmag separation 0
     observing conditions: Global Defaultresources:
D4-MMM-1822:16:34.125-17:47:01.162K_AB=251.5 hours
     S3211320197 (oiwfs)22:16:34.142-17:47:01.7313.37 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-1922:16:54.806-17:42:04.921K_AB=251.5 hours
     S3211120292 (oiwfs)22:16:54.835-17:42:04.7913.35 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D4-MMM-2022:15:46.339-17:50:43.751K_AB=251.5 hours
     S3211320214 (oiwfs)22:15:46.326-17:50:44.1812.96 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-102:24:21.620-04:42:10.938K_AB=251.5 hours
     S00203004 (oiwfs)2:24:21.626-4:42:11.2912.49 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-202:24:14.972-04:24:34.590K_AB=251.5 hours
     S0020111194 (oiwfs)2:24:14.994-4:24:33.9812.55 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-302:26:45.532-04:43:01.495K_AB=251.5 hours
     S002030351 (oiwfs)2:26:45.523-4:43:02.8899.90 Fmag separation 0.02
     observing conditions: Global Defaultresources:
D1-MMM-402:26:57.741-04:37:49.635K_AB=251.5 hours
     S002030321 (oiwfs)2:26:57.743-4:37:50.7512.63 Fmag separation 0.02
     observing conditions: Global Defaultresources:
D1-MMM-502:25:14.493-04:14:47.440K_AB=251.5 hours
     S0020111186 (oiwfs)2:25:14.455-4:14:47.7412.82 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-602:26:11.566-04:58:50.857K_AB=251.5 hours
     S0020303103 (oiwfs)2:26:11.565-4:58:51.0813.00 Fmag separation 0
     observing conditions: Global Defaultresources:
D1-MMM-702:27:07.466-04:59:26.789K_AB=251.5 hours
     S0020303106 (oiwfs)2:27:07.496-4:59:27.7913.07 Fmag separation 0.02
     observing conditions: Global Defaultresources:
D1-MMM-802:27:53.480-04:08:42.499K_AB=251.5 hours
     S002030295 (oiwfs)2:27:53.487-4:08:42.8312.90 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-902:27:18.477-04:04:10.201K_AB=251.5 hours
     S002030286 (oiwfs)2:27:18.508-4:04:10.6113.12 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1002:26:48.776-04:24:26.997K_AB=251.5 hours
     S00203021119 (oiwfs)2:26:47.46-4:24:17.3118.42 Fmag separation 0.37
     observing conditions: Global Defaultresources:
D1-MMM-1102:25:22.327-04:37:14.159K_AB=251.5 hours
     S002030316 (oiwfs)2:25:22.328-4:37:14.4613.11 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1202:26:23.872-04:20:35.285K_AB=251.5 hours
     S0020302130 (oiwfs)2:26:23.88-4:20:35.7513.29 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1302:27:43.555-04:32:57.233K_AB=251.5 hours
     S0020302173 (oiwfs)2:27:43.562-4:32:57.3712.85 Fmag separation 0
     observing conditions: Global Defaultresources:
D1-MMM-1402:24:08.989-04:31:10.873K_AB=251.5 hours
     S0020113190 (oiwfs)2:24:08.997-4:31:11.113.38 Fmag separation 0
     observing conditions: Global Defaultresources:
D1-MMM-1502:25:04.481-04:48:07.293K_AB=251.5 hours
     S002030371 (oiwfs)2:25:04.487-4:48:07.5912.61 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1602:26:54.744-04:41:00.972K_AB=251.5 hours
     S002030341 (oiwfs)2:26:54.759-4:41:01.8113.29 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1702:27:33.833-04:52:40.491K_AB=251.5 hours
     S002030382 (oiwfs)2:27:33.833-4:52:40.8513.26 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-1802:24:30.215-04:38:17.071K_AB=251.5 hours
     S002030324 (oiwfs)2:24:30.227-4:38:17.2713.07 Fmag separation 0
     observing conditions: Global Defaultresources:
D1-MMM-1902:27:15.421-04:08:45.485K_AB=251.5 hours
     S002030296 (oiwfs)2:27:15.448-4:08:45.7613.36 Fmag separation 0.01
     observing conditions: Global Defaultresources:
D1-MMM-2002:25:35.162-04:23:09.947K_AB=251.5 hours
     S00203021232 (oiwfs)2:25:34.403-4:22:54.0417.74 Fmag separation 0.33
     observing conditions: Global Defaultresources:

Resources

Observing Conditions
NameImage QualitySky BackgroundWater VaporCloud Cover
Global DefaultAnyAnyAnyAny

Scheduling Information:

Synchronous dates:

Optimal dates:

Impossible dates:


Additional Information


Keyword Category: Extra Galactic

Keywords: Dynamics, Elliptical galaxies, Galaxy morphology, Interacting galaxies, Multiwavelength study, Starburst galaxies, Stellar populations in external galaxies, Survey

Publications:


Proposal Contents

Summary
Investigators
Abstract
Science Justification
Technical Justification
Observation Details
Allocation Committee Comments
Additional Information