I would like to add a few more words regarding the so-called "Marano
South" field
as a candidate for our verification field. This is a field that I suggested
in
our first meetings as an alternate candidate for the CDF-South because
it was observed
in a large number of wavelengths and it will also be observed in deep
hard X-rays
with XMM (Guaranteed Time). So I am clearly in favor of this field
as a verification
field.
However, there is a risk of confusion regarding this field since several
fields
in the same region were given this same "Marano Field":
(1) the original "Marano Field" was first observed in the optical by
Marano et al.
(1988, ESO 3.6m plates in UJF) then in:
- X-rays (ROSAT + XMM guaranteed time)
- Optical-CCD (ESO EMMI-NTT UBVR)
- VLT FORS2 & ISAAC optical & NIR spectroscopy
- NIR (K, J)
- MIR (6.75 & 15 microns, Ultra-Deep field 9'x9')
- Radio (ATCA at 1.4 & 2.4 GHz)
(2) Another field shifted by 20 arcminutes from the previous field was
selected
because of its lower cirrus emission in order to optimize its observation
in the far
infrared (170 microns with ISOPHOT) for the FIRBACK program.
We usually call this field "Marano FIRBACK 1" and it has a size of 30'x30'.
It was observed in:
- optical (BVRI ESO WFI)
- VLT FORS2 & ISAAC optical & NIR spectroscopy
- MIR (6.75 & 15 microns, Deep (30'x30') and Ultra-Deep (9'x9')
fields)
- FIR (170 microns)
- Radio (ATCA at 1.4 & 2.4 GHz)
(3) A band of 3 extra 30'x30' fields were observed by ISOPHOT at 170
microns
in the framework of the FIRBACK program, which do not overlap with
the deep MIR
images:
- optical (BVRI ESO WFI: not yet analyzed)
- FIR (170 microns)
- Radio (ATCA at 1.4 & 2.4 GHz)
In case the Marano Field appears to be a "GOODS candidate" for our verification
field,
we would have to decide which one between the "Marano Field" proper
and the
"Marano FIRBACK 1" is best suited.
--------------------
MARANO FIELD PROPER:
--------------------
GOODS points:
-------------
The advantage of the "Marano Field" proper is that it was observed
in
X-Rays from soft to hard X-rays with both ROSAT and XMM, and that it
contains NIR images which can be used for our discussion of
optical-NIR information versus MIR-24 microns fluxes.
BADS points:
------------
One inconvenient is that the 6.75 microns ISOCAM image there is
shallower than the one in the "Marano FIRBACK 1" (0.2 instead of 0.05
mJy). However, we are mainly interested in the 15 microns images which
is closer to 24 microns.
-----------------
MARANO FIRBACK 1:
-----------------
GOODS points:
-------------
The advantage here is that it contains 170 microns data and its zodiacal
emission is fainter than in the Marano Field Proper. This difference
did not
affect the 15 microns images but was considered as non negligible for
the FIR
data.
BADS points:
------------
- Bad spatial resolution at 170 microns.
- Absence of X-ray data for the separation AGN/starbursts: we are not
supposed
to make a scientific use of these data but if one can be done, I guess
this
would be goods for SIRTF. Technically though, it may be interesting
to have
a better idea of the fraction of AGNs in the 24 microns sample in comparison
with model expectations because these may also play a role in the definition
of the confusion level...
- nor NIR data...
You will find below more detailed information concerning observations
on these
fields.
Cheers,
David
--------------------------------------------------------------------------------
Marano ROSAT (original Marano Field)
--------------------------------------------------------------------------------
X-Ray:
------
ROSAT:
------
Hasinger G., Burg R., Giacconi R., et al., 1993, A&A 275, 1 (erratum
A&A, 291, 348)
Hasinger G., Burg R., Giacconi R., et al., 1998, A&A 329, 482
Deep 0.5-2 keV X-ray survey (3.7x10^-15 erg/s/cm^2) centered at:
RA(2000)= 03 15 09
DEC(2000)=-55 13 57
XMM:
----
Guaranteed time (Watson, Turner)
Optical:
--------
(See Zamorani et al. 1999, A&A 346, 731)
CCD exposures (EMMI-NTT) in U (down to 23.5) ,B (25), V (24) and R
(24)
over a field centered at:
RA(2000)= 03 15 00
DEC(1950)=-55 25 00
with a radius of ~ 13 arcmin
ESO 3.6m plates (U, J, F bands down to 22 mag)
(Marano et al. MNRAS 232, 111, 1988)
centered on:
RA(2000)= 03 13 08
DEC(1950)=-55 25 00
NIR (Lowenthal, Koo):
---------------------
Two modes using CTIO:
A deep mode in K (to K=19.2, 5sigma) and in J,
area=25'x25', centered at:
RA(2000)= 03 14 30.6
DEC(2000)=-55 17 18
and a shallow mode only in K (to K=16, 5sigma)
of 1 degree x 1 degree centered:
RA(2000)= 03 13 45.0
DEC(2000)=-55 27 38
RADIO: Gruppioni et al. (1997, MNRAS 286, 470)
------
ATCA (Australia Telescope Compact Array) observations centered at:
RA(2000)= 03 15 09.0
DEC(2000)=-55 13 57
at 1.4 and 2.4 GHz down to a sensitivity limit of 0.2 mJy in both bands
(5-sigma).
MIR:
----
ISOCAM Ultra-Deep Survey (9'x9') at 6.75 and 15 microns down to 0.2
and 0.25 mJy
respectively.
Centered on:
RA(2000)= 03h 14m 45s
DEC(2000)=-55d 19m 27s
Spectroscopy:
-------------
Zamorani et al.
Elbaz et al.: VLT FORS2 (~30 galaxies) and ISAAC (time allocated for
next semester)
--------------------------------------------------------------------------------
Marano FIRBACK: 03:13:09.6 -55:03:44 (2000)
--------------------------------------------------------------------------------
Optical:
--------
Wield Field Imager (WFI, ESO) CCD images down to V~24 in BVRI of the
whole
1 square degree observed with ISOPHOT at 170 microns.
Radio:
------
Dole et al. (in preparation): ATCA (Australia Telescope Compact Array)
observations
at 1.4 & 2.4 GHz, sensitivity: to be determined (sub-mJy I guess).
MIR:
----
ISOCAM Ultra-Deep Survey (9'x9') at 6.75 and 15 microns down to 0.05
and 0.25 mJy
respectively. Also Deep Survey (28'x28') at 15 microns down to
~0.4 mJy.
Centered on:
RA(2000)= 03h 13m 9.6s
DEC(2000)=-55d 03' 44"
FIR:
----
ISOPHOT 170 microns in 4 fields of 30'x30' each. One of which is centered
on
the same field as the ISOCAM Deep & Ultra-Deep surveys at 6.75
and 15 microns
Spectroscopy:
-------------
Elbaz et al.: VLT FORS2 (~30 galaxies) and ISAAC (time allocated for
next semester)