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"The best observing practice is to adopt a star and stick to it - *density of observation* is very critical.  Until you don't like it any more - then adopt a different star!" --Joe Patterson (Columbia University, CBA boss)

Our first observing priority are accreting white dwarfs which have been observed to host classical nova explosions. As Joe Patterson said on 2016 Apr 25, A word about this project - the long-term "old nova project". We'd like to track the evolution of nova orbital light curves, over the first few decades after outburst. The most interesting interval is the first few years, so even very recent novae (say 1-3 years) are eligible. Most novae flash orbital light curves, and most show a very characteristic light curve, suggesting heating of the secondary - a double-sinusoid with an apparent eclipse. In theory, the evolution of the "eclipse" and the double wave allows deduction of the changing pattern of heating in the binary... and that might even allow us to track the cooling of the white dwarf, decades after eruption.

Last updated by Laura Chomiuk on 2018 May 23.

Exoplanets Edit

KELT Transit Finder- There won't be set comparison stars for these. Just choose 3 stars in your field that have similar brightness as your target star, and note their x/y positions. Try get an hour before and/or after the transit, and make sure to make a finder chart of your field.

Binaries and Cataclysmic Variables Edit

V959 Mon: RA = 06 39 38.74, Dec = +05 53 52.0 Edit

  • Finder chart
  • Nova that exploded in 2012 that is near and dear to Laura's heart
  • This one is pretty faint, ~17.3 mag. You might need to do few minute exposures in clear filter, and probably need decent seeing. If you decide it's REALLY too faint and not doable after trying, please make a comment here so we can officially retire it.

V1062 Tau: RA= 05:02:27.47, Dec= +24:45:23.3 Edit

Nova Outbursts Edit

Nova V392 Per: RA=04:43:21.37, Dec=+47:21:25.9 Edit

  • Finder chart
  • Please get nice B, V, R, I exposures (say, just three exposures in each filter) every night you observe and the source is visible in the sky (it's probably mostly set for summer 2018, but should be visible again in late 2018). You don't need to sit on this one for monitoring sequences.
  • Don't need to submit to CBA; these are for Laura! Send to chomiuk-AT-pa.msu.edu instead

Nova ASASSN-17hx: RA=18:31:45.918, Dec= -14:18:55.57 Edit

  • PLEASE still observe this, in Summer 2018!!! This source is still bright, at V~12.5 mag, and other folks aren't observing it!
  • Finder chart
  • Please get nice B, V, R, I exposures (say, just three exposures in each filter) every night you observe and the source is visible in the sky. You don't need to sit on this one for monitoring sequences.
  • Comparison Star: 127
  • Check Star 1: 134
  • Check Star 2: 120
  • Don't need to submit to CBA; these are for Laura! Send to chomiuk-AT-pa.msu.edu instead

Retired (at least presently): Edit

FS Aur: 05:47:48.36, +28:35:11.2

Paloma=RX J0524+4244: 05:24:30.44, +42:44:50.8

DW Cnc: 07:58:53.07, +16:16:45.4

  • Finder chart
  • More info on Koji's intermediate polar (IP) page
  • 1.4 hour orbital period; 39 minute white dwarf spin period.
  • "DQ Her"-like, or an intermediate polar. So the white dwarf has a pretty strong magnetic field.
  • Should be in the range 15--17.5 mag. So either V band or clear monitoring may work; if you have opinions on which is better, report back!

YZ CNC: 08:10:56.65, +28:08:33.2

  • Finder chart
  • Variable Type: SU UMa type dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: V
  • Exposure Length: not specified
  • Orbital Period: 2.08 hours
  • Outburst Period: 7-10 days
  • Superoutburst Period: 100-110 days
  • Quiescence Magnitude: 14.8
  • Outburst Max Magnitude: 12.0
  • Superoutburst Max Magnitude: 11.0

CR Boo: 13:48:55.22, +07:57:35.8

  • Variable Type: AM CVn type dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: Clear
  • Exposure Length: not specified
  • Quiescence Magnitude: ~15.0

OV Boo: 15:07:22.35, +52:30:39.8

ES Dra: 15:25:31.81, +62:01:00.0

  • Variable Type: Z Cam dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: V (Clear if too dim)
  • Exposure Length: not specified
  • Period: 4.2 hours
  • Quiescence Magnitude: 15.4
  • Negative Superhump Magnitude: 17.0
  • Finder chart

IGR J19552+0044: 19 55 12.47 +00 45 36.6

  • Finder chart
  • Short exposures (as short as possible!)
  • Comparison Stars: 148, 145, 158

V2306 Cyg: 19 58 14.46 +32 32 42.4

Nova V339 Del: RA= 20 23 30.73  Dec= +20 46 04.1

  • This is a nova that went off in 2013 that is still optically bright, at V ~ 14.5 mag. We want to monitor it to see if we can find the binary period.
  • Observe this one in V band for long time series.
  • Finder chart

V2069 Cyg: 21 23 44.83 +42 18 01.6

V598 Peg = RX233325.92+152222: 23:33:25.99, +15:22:22.2

FY Per: RA= 04 41 56.60, Dec= +50 42 36.0

  • FY Per is a total mystery star. A well-determined spectroscopic period of 0.2585 d, but every so often, a 90-minute photometric period pops up just a few hundredths of a magnitude, but not particularly difficult to study since the star is 12th mag. One of these years, we should figure it out!
  • Finder chart
  • Nice long sequences on this guy, preferably in V filter.
  • Comparison stars: 136 V: 13.612, 135 V: 13.478, 143 V: 14.34

FO Aqr: 22:17:55.38, -08:21:03.8

  • Use a 'clear' filter and take short exposure (<60 seconds), as you are trying to resolve an 11 minute period

BY Cam: RA = 05 42 48.80, Dec = +60 51 31.4 Edit

  • Finder Chart
  • Comparison Stars (In Order): 130 V: 12.969, 148 V:14.789, 134 V:13.392
  • Filter: Clear

DQ Her: RA = 18 07 30.3, Dec = +45 51 33

  • Filter: Clear

AM CVn: RA = 12:34:54.62, Dec = +37:37:44.1

  • Finder Chart
  • Comparison Stars (In Order): 144, 157, 125
  • Filter: Clear
  • Magnitude: 14-14.5

HP Lib: RA=15:35:53.07, Dec = -14:13:12.2

  • He-rich cataclysmic variable, should be around 13.5 mag
  • Finder chart

SDSS J141118.31+481257.6: RA= 14:11:18.32, Dec= +48:12:57.5

  • This AM CVn-type variable is currently undergoing its first recorded outburst (12.6 mag, detected by Tadashi Kojima on 2018 May 19.514 UT). Time-resolved photometry is urgently required.
  • comp star 1: 127
  • comp star 2: 139

ASASSN-18ey: RA= 18:20:21.95, Dec=+07:11:07.3

  • HIGH PRIORITY SUMMER 2018
  • New X-ray transient, with powerful super humps
  • Joe Patterson recommends using V filter
  • recommend longer exposures
  • Finder chart
  • Use comparison stars: 146, 128, 143

V1974 Cyg: 20:30:31.61, +52:37:51.3

  • Finder chart
  • Use comparison stars 139, 142, 146
  • Filter to use: Clear

AO Psc: RA= 22:55:17.896, Dec= -03:10:39.98

  • Finder Chart
  • Use comparison stars: 97, 114, 143
  • Filter to use: Clear

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