Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-South Field, Non-SNe-Searched Visits
The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS)
is designed to document the first third of galactic evolution from z =
8 to 1.5 via deep imaging of more than 250,000 galaxies with WFC3/IR
and ACS. It will also find the first Type Ia SNe beyond z > 1.5 and
establish their accuracy as standard candles for cosmology. Five
premier multi-wavelength sky regions selected from the Spitzer
Extragalactic Deep Survey (SEDS) provide complementary IRAC imaging
data down to 26.5 AB mag, a unique resource for stellar masses at all
redshifts. The use of five widely separated fields mitigates cosmic
variance and yields statistically robust and complete samples of
galaxies down to 10^9 solar masses out to z ~ 8.
The program merges two originally separate MCT proposals. The Faber
program incorporates a “Wide” imaging survey in three separate fields
to ~2 orbit depth over ~0.2 sq. degrees, plus a “Deep” imaging survey
to ~12 orbit depth in the two GOODS regions over ~0.04 sq. degrees.
When combined with ultra-deep imaging from the Hubble Ultradeep Field
program (GO 11563), the result is a three-tiered strategy that efficiently
samples both bright/rare and faint/common extragalactic objects. The
Ferguson program adds an extensive high-redshift Type Ia SNe search,
plus ultraviolet "daytime" UVIS exposures in GOODS-N to exploit the
CVZ opportunity in that field.
This program, GO 12060, is part of the GOODS-S Deep survey. Special Deep
science highlights include:
* Detection and counts of early galaxies to z ~ 7-8 as revealed
by red-sensitive WFC3-IR images beyond the Lya break
- Measurement of the luminosity function of infant galaxies
down to 10^9 solar masses out to z = 7-8
- Measurement of the faint-end LF slope to assess the
contribution of faint galaxies to cosmic reionization
* The physics of early star formation
- Propertes of the earliest star-forming regions -- sizes,
star-formation rates, stellar masses and radiation densities,
dust contents
- In concert with Spitzer/IRAC data, measurement of the key
relation between star-formation rate and stellar mass --
what set the rate of early star formation in galaxies?
- When did star-formation begin to slow down? In what types
of objects? Why?
* Structural properties, stellar masses, and environments of the
earliest identifiable non-QSO AGN as revealed by WFC3-IR
* Structure of highly reddened, dust-obscured galaxies
* Deep imaging of the outer envelopes of galaxies
- Evidence for galaxy-galaxy interactions; counts of merging
galaxies
- Growth of the outer envelopes and evolution of structure
of spheroidal galaxies
* Search for Type Ia SNe to z ~ 2 exploiting the long-wavelength
J and H sensitivity of WFC3-IR. The first comprehensive
search for Type Ia's at these large distances and early epochs.
GOODS-S Overview:
The CANDELS program in Cycle 18 includes:
GO 12060: Deep mosaic in GOODS-S: Y-band + one skirt epoch
GO 12061: Deep mosaic in GOODS-S: J+H, epochs 1-5 + 2 skirt epochs
GO 12062: Deep mosaic in GOODS-S: J+H, epochs 6-10
GO 12063: Wide mosaic in Extended Groth Strip (EGS)
GO 12064: Wide mosaic in UKIDSS/Ultradeep Survey (UDS)
Field maps and details are at http://candels.ucolick.org.
Program GO 12060 executes the Y-band observations in GOODS-S, which
are not designed specifically for SNe search (though some may be
found). One epoch of skirt observations is also included.
GOODS-S observations are in two flavors: 1) the Deep area proper,
which covers approximately 3x5 WFC3-IR tiles and runs east-west near
the middle of the GOODS-S region, and 2) the "skirt", which contains 9
tiles in a roughly rectangular pattern running parallel to Deep but
offset to the south. The transverse layout of Deep matches the
deepest IRAC data in GOODS-S, which are needed for stellar masses. The
Deep region and its skirt coordinate with one another and with
existing WFC3 and ACS data to achieve the observational goals of the
GOODS-S Deep program, as follows:
1) Detect z ~ 7-8 galaxies down to 0.5L* by imaging the Deep area to
an *effective* depth of 4 orbits in WFC3-IR F125W and F160W and 3
orbits in Y. The reduction to 3 orbits in Y frees up 15 orbits for
the skirt area without impacting the SNe search (Y is not prime for
SNe) and was tested with extensive sensitivity simulations. The
actual number of orbits used for J and H is 5 in order to allow for
the inclusion of F350LP exposures in WFC3-UVIS for SNe rejection (see
below), hence the term "effective" for the J and H exposure times.
2) Provide at least 32,000 s of exposure time in F814W at each point
within the Deep area. This is needed to establish the Lya break in
distant z ~ 7-8 galaxies and is essential for discriminating them from
reddened foreground galaxies at z ~ 2. The quota for F814W is met by
adding together ACS parallels from the present program (GO 12060-2) to
parallels in existing F814W exposures plus future F814W exposures
that are planned in GO 11563. A considerable fraction of the ACS
parallel coverage on Deep comes from parallels that originate from the
skirt region, which has been placed to the south to balance ERS2 to
the north and additionally increases total WFC3-IR coverage in GOODS-S.
3) Maximize the number of J and H orbits usable for SNe searching.
SNe are discovered in J and H, but low-redshift interlopers and other
SNe types are rejected using short-wavelength ACS exposures taken
close in time. These should preferably be taken within 3 days of J/H.
The short-wavelength exposure can in principle be provided by 1300 s
in contemporaneous F606W ACS parallels, but in practice these are not
available over most of GOODS-S, and so a short ~430 s F350LP UVIS
exposure is inserted into the J/H orbit instead. The follow-up for
discovered SNe is provided in GO 12099.
Meeting the above requirements creates a complex interlocking puzzle
in which one must lay out two seamless mosaics to the required depth
in both the Deep and skirt areas, locate and orient them to match
existing data (e.g., IRAC), have ACS parallels lie on top of the
WFC3-IR area as much as possible, reach the desired minimum exposure
time of 32,000 s in parallel F814W in the Deep area, use any excess
parallel exposure time beyond this productively, take Deep data at
multiple epochs spaced ~52 d apart for SNe searching, operate within
the narrow range of ORIENTs available at each epoch, allow for at
least 30 days of SNe follow-up time after each SNe search epoch,
identify suitable guide stars for all observations, break up each
orbit into enough exposures to produce a reasonable dither pattern but
not waste too much time in extra readouts, and work around solar
avoidance, which removes ~60 degrees and two months of calendar
time in April-May from the available ORIENTs. The final design was
adopted after exploring many possibilities and represents a
compromise. It is generally impossible to perturb any aspect of the
program significantly without adversely impacting several others.
Details of GOODS-S observations:
* Filters used: Y = F105W, J = F125W, H = F160W, V = F606W, I = F814W,
z = F850LP
* Deep area, J and H exposures:
- 10 1-orbit epochs lasting from Oct 2010 to Feb 2012
- Nominal WFC3-IR exposure times per orbit: 1/2 orbit J, 1/2 orbit
H, each broken into two sub-exposures. J and H are co-added
for SNe searching; the four exposures yield a good dither pattern
- F350LP inserted for low-z SNe rejection
- Total effective exposure time allowing for F350LP: 4 orbit depth
in J, 4 orbit depth in H
- 10 epochs span solar avoidance gap of ~50 days, permit 8 prime
SNe search epochs with 52 d cadence plus one less sensitive
search across solar avoidance gap
* Skirt area, J and H exposures:
- Two 1-orbit epochs taken in Jan 2011 and Feb 2011
- Nominal WFC3-IR exposure times per orbit: 1/3 orbit J, 2/3 orbit H,
each one broken into two sub-exposures (mimics Wide mosaics in other
fields)
- 2 epochs permit one epoch of SNe search on each skirt tile
* Deep and skirt areas, Y:
- 3 orbits in Deep, to complement 4-orbit J+H there
- 1 orbit at another epoch in skirt, to complement 2-orbit J+H there
- All epochs chosen to throw ACS parallels maximally onto Deep
* SNe search combines all J and H exposures from each epoch into a
single image. Small-scale four-point dither treats them as part
of same exposure, gives sub-pixel sampling
* ACS parallels lying completely or largely within the Deep area:
- Default filter is I-band with goal of obtaining at least 32,000
sec of exposure time at virtually all locations within the Deep
area. Sum includes all known past and future I exposures from
other programs at that field location. Getting sufficient I
takes precedence over getting V in a contemporaneous parallel if
total I goal is not met
- Next goal is one orbit (~2500 sec) of z, for variability studies.
Again, this takes precedence over V parallel
- If above goals are met, take up to two orbits (5,000 s) of V
- If still more time is left, put into I
* ACS parallels lying largely outside the Deep area:
- First goal is to get one orbit (2500 sec) of I everywhere
- Second goal is to get one orbit (2500 sec) of z for variability studies
- If still more time, put into 2/3 I and 1/3 V to mimic the balance
in the Wide mosaics
* Gap from early April to late May due to solar avoidance:
- The gap in 2011 is Apr 7 - May 27 inclusive (50 d)
- 30 d are budgeted for SNe searching after the last search epoch
before solar avoidance (Epoch 4)
- Deep epochs before solar avoidance are covered by GO 12061.
Both skirt J/H epochs are also included in GO 12061
- Deep epochs after solar avoidance are covered by GO 12062.
There are no skirt epochs in GO 12062
Specifics of GO 12060:
* Y in the Deep area:
- Since Y-band is not used to search for SNe, Y exposures can
be tuned to throw their parallels onto Deep. Y is a major
source of parallels for Deep
- 3-orbit exposures are taken at each location, all at the same visit
and ORIENT
- The 3x5 Y-band mosaic covers the Deep area and is divided
into two epochs:
- 2x3 tiles are observed at one epoch (Jun 2011), 3x3 tiles at
a second epoch 180 deg apart (Nov-Dec 2011). Both epochs throw
parallels onto the Deep area. The mosaic is seamless except:
- Tile 3I is shifted south to find a guide star
- Tile 3R is rotated slightly to put its ACS parallel in an
underobserved part of Deep
- Tile 3P is rotated to find a guide star
- The chosen mosaic overlap is 4%, which yields a minimum overlap
of 1% (1.3") in the short direction to defend against estimated
pointing errors of ~0.2-0.25"
- ? dither pattern
* Y in the skirt area (Mar 2011):
- The skirt consists of 8 WFC3-IR tiles in a 2x4 array, plus three
additional J+H tiles that were added to boost ACS parallel coverage
in underserved parts of the Deep region
- The skirt array is offset to the south of the Deep area and runs
parallel to it (east-west)
- Parallels from the skirt overlie the Deep region as much as possible
- 1-orbit Y exposures are taken at each skirt location
- The chosen mosaic overlap is again 4%
- The three extra J+H tiles (4B, 4C, 4D) consist of 1/3 orbit J and
2/3 orbit H to match the other J+H skirt observations
- ? dither pattern
* Timing
- Y is not designed to search for SNe. The observations can be
taken any time that the desired ORIENTs are available.
The specified ORIENTs are needed to create mosaics that are as
seamless as possible given the guide star constraints
Comments for schedulers:
Guide stars:
* Guide stars have been pre-screened. Use of "SINGLES" is approved by
the PI.
BETWEENs and ORIENTs:
* The BETWEEN epochs are chosen to place all ACS parallel coverage as
much as possible on top of the Deep region
* The ORIENTS are identical to get seamless WFC3-IR mosaics
* A few tiles are rotated or displaced in order to get guide stars
* There are no other timing requirements besides BETWEEN/ORIENT
Bright objects -- persistence:
* The Deep Y-band exposures will be pushed to the deepest possible
limiting magnitude. Please do not schedule bright objects (like
star clusters) in the 8?-orbit window before our observations
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