David R. Ciardi NExScI/IPAC/Caltech
2014 August 29
Kepler/K2
iPTF
Telescope
1m Schmidt
1m Schmidt
Field of View
10o x 10o (100 sq. degrees)
3.5o x 2.3o (7.26 sq. degrees)
Postage stamps
Full frames
Pixel Scale
4”/pixel
1.01”/pixel
Observing
Cadence
30 minutes for most targets
1 minute for ~10% targets
60 seconds integration time but flexible.
Sampling flexible but typical experiments
have been 90 seconds to 5-days sampling
Field Duration
~70 – 80 days
Flexible but generally any one field is
available for months depending on
declination.
Data
availability
Pixel data available a few months Data available in real time
after end of campaign
Orientation
Aligned with ecliptic
8/28/2014
Aligned in equatorial coordinates
2
8/28/2014
18-20 iPTF Pointings
3
8/28/2014
4
8/28/2014
5
8/28/2014
6
Field Observed R.A.
by Kepler
Dec.
PTF g
PTF r Dates Observed by PTF
Kepler
2009 - 2014
19:22:40.00 +44:30:00.0
119
50
3/16/11-9/27/12
K2 0
2014 Apr 30 06:33:11.14 +21:35:16.4
17
16
3/28/10-3/26/14
K2 1
2014 Jul 22
11:35:45.51 +01:25:02.3
0
22
5/24/13-3/8/14
K2 2
2014 Oct 14 16:24:30.34 -22:26:50.3
0
2
2/26/10-2/26/10
K2 3
2015 Jan 05
22:26:39.68 -11:05:48.0
0
21
6/26/09-8/28/10
K2 4
2015 Mar 29 03:56:18.22 +18:39:38.1
0
47
8/24/10-2/18/14
K2 5
2015 Jun 20 08:40:37.84 +16:49:46.6
0
69
1/18/09-5/19/14
K2 6
2015 Sep 11 14:01:11.20 -13:16:02.8
0
0
null
K2 7
2015 Dec 03 19:34:16.22 -22:38:23.4
0
19
7/27/11-6/16/13
K2 8
2016 Feb 24 01:04:43.18 +05:11:52.2
0
38
7/8/10-11/2/12
K2 9
2016 May 17 18:23:35.72 -24:12:12.8
0
23
7/3/14-8/15/14
8/28/2014
7
Field
Kepler
K2 0
K2 1
K2 2
K2 3
K2 4
K2 5
K2 6
K2 7
K2 8
K2 9
Galactic
Longitude
Galactic
Latitude
76
191
264
354
51
172
209
327
16
129
8
13
6
58
18
-52
-25
32
46
-20
-57
-5
Notes
Original Kepler Field
Low latitude, anti-center
North Galactic Cap
Near Galactic Center, rho Oph, U. Sco
South Galactic Cap
Pleiades, Hyades
M44, M67
North Galactic Cap
Near Galactic Center
South Galactic Cap
Galactic Center, Baades Window – mlens!!
All fields at low ecliptic latitude (< 1 degree from ecliptic) – good for solar system!
8/28/2014
8
Campaigns start
a maximum of 52
days before each
date and end no
later than 30 days
after each date.
8/28/2014
9




Northern Fields easier to do
Most southernly fields (declination ~ -25o) just
barely get above airmass of 2 (Fields 2, 7, 9)
Fields 3 and 6 climb above 2 airmass but not for
long (declination ~ -12o)
Amount of time fields are available for
simultaneous observations depends upon field
but is typically 10 - 30 days at the beginning of
a campaign
8/28/2014
10


8/28/2014
Started 22 Aug
Because of low
declination, never
gets above 2
airmass during
the K2
observation
window
11


8/28/2014
Starts early/midFebruary
Because of higher
declination
available with
PTF for first 30-40
days depending
on exact field start
with Kepler
12



Winter fields most
accessible – but
they precede the
K2 observations.
Otherwise, fields
are available about
6 – 7 months after
K2 campaign
Good timing for
enabling of followup
8/28/2014
13



Hard to do preparatory observations because of
time cycle of proposals
Targets for Fields 4 and 5 due now (late
September)
Fields 6 and 7



First observable Feb/Mar 2015
Proposals due end of Feb 2015
Fields 8 and 9

First Observable
 Field 8: Jun/Jul 2015
 Field 9: Apr/May 2015


8/28/2014
Proposals due end of July 2015
But Field 9 is special
14




Points ahead of the
Earth
Field available
from ground
throughout the
campaign
mlens events
observed from
Earth and Kepler
yields parallaxes
5 sq deg. dedicated
to mlens; 15% to
other GO targets
8/28/2014
15






Wide-field multi-band photometry
High cadence time series photometry
Seeing-limited resolution
Pre or Post SED characterization
Pre or Post or Simultaneous time series data
complementary to K2
Photometric Deblending of K2 targets
8/28/2014
16


K2 observing about 10
clusters
Need supporting
observations to determine




Need wide-field of view
Deep observations to get to end
of the main sequence
Cluster membership (colormagnitude diagram)
Deblending (higher resolution
imaging)
8/28/2014




Pleiades
Hyades
M44
M67 …
 To Name a Few
17




K2 Fields are all in the ecliptic!
NEOs and asteroids move too much
between discovery, K2 proposal process,
and start of K2 observations
Slow moving objects discovered by PTF
may stay in field long enough to be
remain in K2 Field (e.g., Trojans, KBOs,
trans-Neputunian objects)
Colors and rotation periods
8/28/2014
18




Quicker time cadence than K2
Multiband, wide-field photometry: deeper and better
resolution than K2
All K2 fields observable with PTF
Only northern fields have realistic chance of
simultaneous PTF/K2 observing



Except for Field 9 which is the mlensing field
PTF may be good for identification of variable objects
worthy of K2 following – if PTF observes the field
soon enough (older data?)
PTF is probably better at following up K2 targets
discovered to be interesting
8/28/2014
19