PACS Evolutionary Probe (PEP) – A Herschel key program

D. Lutz; A. Poglitsch; B. Altieri; P. Andreani; H. Aussel; S. Berta; A. Bongiovanni; D. Brisbin; A. Cava; J. Cepa; A. Cimatti; E. Daddi; H. Dominguez-Sanchez; D. Elbaz; N. M. Förster Schreiber; R. Genzel; A. Grazian; C. Gruppioni; M. Harwit; E. Le Floc’h; G. Magdis; B. Magnelli; R. Maiolino; R. Nordon; A. M.  Pérez García; P. Popesso; F. Pozzi; L. Riguccini; G. Rodighiero; A. Saintonge; M. Sanchez Portal; P. Santini; L. Shao; E. Sturm; L. J. Tacconi; I. Valtchanov; M. Wetzstein; E. Wieprecht

doi:10.1051/0004-6361/201117107

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Volume 532 (August 2011)

A&A, 532 (2011) A90

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Table 1

PEP fields.

Field	RA	Dec	Size	PA	Wavelengths	Observations	Time
	degree, J2000		arcmin	degree	μm		h

COSMOS	150.11917	2.20583	85 × 85	0^a	100,160^b	Nov. 2009–Jun. 2010	196.9
Lockman Hole XMM	163.17917	57.48000	24 × 24	0	100,160^b	Oct. 2009–Nov. 2009	32.1
EGS	214.82229	52.82617	67 × 10	40.5	100,160^b	May 2011–June 2011	34.8
ECDFS	53.10417	–27.81389	30 × 30	0	100,160^b	Feb. 2010–Feb. 2011	32.8
GOODS-S	53.12654	–27.80467	17 × 11	–11.3	70,100,160^b	Jan. 2010	239.7
GOODS-N	189.22862	62.23867	17 × 11	41	100,160^b	Oct. 2009	25.8
Cl0024+16	6.62500	17.16250	6 × 6	45^c	100,160^b	Jun. 2010	6.2
Abell 370	39.97083	–1.57861	4 × 4	45^c	100,160^b		5.3
MS0451.6-0305	73.55000	–3.01667	4 × 4	45^c	100,160^b	May 2010	5.3
Abell 1689	197.87625	–1.34000	4 × 4	45^c	100,160^b	Jan. 2011–	13.0
RXJ1347.5-1145	206.87708	–11.75250	4 × 4	45^c	100,160^b	Feb. 2011	5.3
MS1358.4+6245	209.97625	62.51000	4 × 4	45^c	100,160^b	May 2010	5.3
Abell 1835	210.25833	2.87889	4 × 4	45^c	100,160^b	Feb. 2011	5.3
Abell 2218	248.97083	66.20611	4 × 4	45^c	100,160^b	Oct. 2009	10.2
Abell 2219	250.08333	46.71194	4 × 4	45^c	100,160^b	May 2010	5.3
Abell 2390	328.40417	17.69556	4 × 4	45^c	100,160^b	May 2010	5.3
RXJ0152.7-1357	38.17083	–13.96250	10 × 5	45	100,160,250,350,500	Mar. 2010–Jan. 2011	5.8
MS1054.4-0321	164.25092	–3.62428	10 × 5	0	100,160,250,350,500	Jun. 2010–Dec. 2010	5.8

Notes. List of the six blank deep fields, ten lensing clusters, and two z ~ 1 clusters to be observed by PEP. As of early June 2011, surveys for all fields except Abell 370 and Abell 1689 are completed (see column “Observations”).

^(a)

Approximate. See Sect. 3 for detailed implementation;

^(b)

250, 350, 500 μm obtained in coordinated observations by the HerMES key program (Oliver et al. 2011);

^(c)

in array coordinates, true position angle on sky will depend for these fields on execution date of the observation.

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