From jop at astro.columbia.edu  Fri Jan  4 05:47:28 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Fri, 4 Jan 2013 05:47:28 -0500 (EST)
Subject: (cba:news) Today's mystery, and stars for January
Message-ID: <6da4040a9f38af1ee9422dfa22bf217c.squirrel@webmail.astro.columbia.edu>

Dear CBAers,

Here's a mysterious object in the morning mail!  Still not enough
information to figure out what astrophysical box to put it in... and might
be a pow'f'l interesting CV.

Here are some recommendations for early January.

GD 552.  Out of season... but still available to borealites, and a star
for which we are just about to ship off our long-term study.  It would be
great to obtain a couple weeks of LONG runs.

T Pyx. Similar story for the south.  Due mainly to Arto's and Berto's
Herculean efforts, we have the main (amazing!) result from our post-nova
timing study - a change in Porb by a whopping 0.006%.  Apparently
signifying a very large ejected mass, inconsistent with our theories of
recurrent novae.  I expect to have the paper ready in a month.  However,
there's some chance that this post-nova period is slightly *changing*,
which could greatly affect the interpretation. Another solid two weeks of
LONG runs could really nail this down - by delivering a very accurate
timing point at the end.  (dP/dt issues usually come down to "how long is
the baseline", and "how accurate are the timings at the start and end of
the data".)

DI UMa needs about another 3 weeks of coverage.  The most important issue
still on the table is: what is that period in quiescence?  Is it Porb, or
a negative superhump, or possibly a long-lived residue of the positive
superhump?  The *stability* of the period will help answer to this.  After
about 3 more weeks, the star will have spanned another quiescence, and we
might learn the answer.

We're done with PX And, MU Cam (for now), and PQ Gem (for now).  We could
definitely use more on RX0704+26, Swift 0732-13, and DW Cnc (need to go
long on the latter, since Pspin could get confused with Porb).

For northern observers who would like to specialize on one star, I
recommend BY Cam - arguably the king of the asynchronous polars.  This
positively needs a LONG campaign... but will definitely yield some nice
publishable results.

For the other ER UMa stars, I'll let Enrique give reports and advice.  Our
ongoing V1159 Ori campaign is definitely going GREAT, and should continue.
I'm not sure about the other three currently well-placed members: RZ LMi,
ER UMa, BK Lyn.

Good luck!

                  Joe



---------------------------- Original Message ----------------------------
Subject: [vsnet-outburst 14957] Re: [vsnet-alert 15238] OT
J122221.6-311525  = bright CRTS transient
From:    "Hiroyuki Maehara" <maehara at kiso.ioa.s.u-tokyo.ac.jp>
Date:    Fri, January 4, 2013 1:39 am
To:      vsnet-alert at ooruri.kusastro.kyoto-u.ac.jp
         vsnet-campaign-dn at ooruri.kusastro.kyoto-u.ac.jp
         vsnet-outburst at ooruri.kusastro.kyoto-u.ac.jp
         vsnet-newvar at ooruri.kusastro.kyoto-u.ac.jp
--------------------------------------------------------------------------

 The object was detected at Vmag=11.8 by the Kyoto/Kiso Wide-field Survey
on Dec 26.

OT_J122221.6-311525 20120328.63044 <11.0V KW2 --
OT_J122221.6-311525 20120328.63083 <11.0V KW2 --
OT_J122221.6-311525 20120331.61500 <10.9V KW2 --
OT_J122221.6-311525 20120331.61535 <10.7V KW2 --
OT_J122221.6-311525 20120407.58847 <10.7V KW2 --
OT_J122221.6-311525 20120407.58882 <10.8V KW2 --
OT_J122221.6-311525 20120414.57725 <11.2V KW2 --
OT_J122221.6-311525 20120414.57762 <11.3V KW2 --
OT_J122221.6-311525 20120417.58544 <9.1V KW2 --
OT_J122221.6-311525 20120417.58581 <9.5V KW2 --
OT_J122221.6-311525 20120427.55866 <11.2V KW2 --
OT_J122221.6-311525 20120427.55903 <11.0V KW2 --
OT_J122221.6-311525 20120428.56146 <10.4V KW2 --
OT_J122221.6-311525 20120428.56181 <10.9V KW2 --
OT_J122221.6-311525 20120512.52359 <11.1V KW2 --
OT_J122221.6-311525 20120512.52396 <10.9V KW2 --
OT_J122221.6-311525 20121226.87655 11.844V KW2 0.245
OT_J122221.6-311525 20121226.87690 11.806V KW2 0.246
OT_J122221.6-311525 20121226.87741 12.020V KW2 0.273

KW2: Kyoto/Kiso Wide-field Survey
     f=105mm lens (F/2.0) + SBIG ST-8XME



On Fri, Jan 04, 2013 at 10:11:35, Taichi Kato wrote:
> OT J122221.6-311525 = bright CRTS transient
>
> SSS130101:122222-311525
http://nesssi.cacr.caltech.edu/SSS/20130101/1301010310804113661.html 12
22 21.63 -31 15 24.9 12.36 No SDSS object CV
>
>    No outburst was recorded in ASAS-3.
>
> ROSAT source:
> 122221.4 -311544 (2000.0) 1RXS-F_J122221.5-311545 0.050 0.75 0.05
>
> ===
>
> ATEL #4699							     ATEL #4699
>
> Title:	Detection of a Bright Optical Transient by CRTS
> Author:	A. J. Drake, S. G. Djorgovski, A. A. Mahabal, M. J. Graham,
> 		R. Williams (Caltech); R. McNaught (ANU); J. Prieto (Princeton); M.
> 		Catelan (PUC Chile); E. Christensen, S. M. Larson (LPL/UA).
> Queries:	ajd at cacr.caltech.edu
> Posted:	4 Jan 2013; 00:24 UT
> Subjects:Optical, Cataclysmic Variable, Transient, Variables
>
> Further to ATel#4678, here we report the CRTS discovery of
> <a
href=http://nesssi.cacr.caltech.edu/SSS/20130101/1301010310804113661.html>SSS130101:122222-311525</a>.
>
> This source was detected at V = 12.3+/-0.1 in four images taken by the
> <a href=http://www.mso.anu.edu.au/~rmn/>Siding Spring Survey</a>
> on 2013-01-01 UT and is located at RA=12:22:21.63 Dec=-31:15:24.9
>
> Based on 230 measurements (from 90 nights of observation between Aug. 2005
> and Aug. 2012), the
> object has an average magnitude of V ~19. The source exhibits variability
> at the
> level of ~1 magnitude in this archival data, yet shows no prior outbursts.
>
> The source is well detected by GALEX (with NUV =18.9+/-0.1 and FUV
19.6+/-0.2)
>
> and may match ROSAT X-ray source 1RXS J122221.5-311545.
> The object is also a very good positional match to radio source NVSS
J122222-311529.
>
> However, it is no clear source is seen in radio observations from the SUMSS
> and VLSS
> surveys.
>
> This large, bright outburst, along with the UV detection and correspondence
> with an X-ray
> source, are most consistent with a cataclysmic variable. However,
association
> with
> a radio source is generally unexpected for CVs and may be coincidental
> or spurious.
> Further observations are required to determine the nature of this event.
>
> A finding chart is available
> <a
href="http://crts.caltech.edu/ATEL/SSS/1301010310804113661.atel.html">here</a>.
>
>





From jop at astro.columbia.edu  Sun Jan  6 20:22:33 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Sun, 6 Jan 2013 20:22:33 -0500 (EST)
Subject: (cba:news) [Fwd: [vsnet-alert 15246] OT J112619.4+084651 = Catalina
	transient]
Message-ID: <558a57578e9fcefe5bd1400ff009cb05.squirrel@webmail.astro.columbia.edu>

DEFINITELY an interesting target.  7 magnitudes is the magic number...
worth a special effort to nail for as long as possible!

joe



---------------------------- Original Message ----------------------------

--------------------------------------------------------------------------

OT J112619.4+084651 = Catalina transient

   CRTS detected a very large amplitude dwarf nova (>7 mag)
CSS130106:112619+084651.  The object is a very good candidate
for a WZ Sge-type dwarf nova.  Observations are encouraged.

SDSS magnitudes: 22.20, 21.83, 21.84, 22.28, 21.31
(no neural net solution for Porb, SDSS i mag may be too faint - eclipsing??)

   No previous outburst was detected in CRTS.

CSS130106:112619+084651
http://nesssi.cacr.caltech.edu/catalina/20130106/1301061090614105661.html
11 26 19.44 +08 46 51.0 14.84
http://skyserver.sdss3.org/dr8/en/tools/chart/navi.asp?ra=171.5809900&dec=8.7808300
CV





From jop at astro.columbia.edu  Tue Jan  8 08:28:16 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Tue, 08 Jan 2013 08:28:16 -0500
Subject: (cba:news) OT J112619.4+084651 again
In-Reply-To: <558a57578e9fcefe5bd1400ff009cb05.squirrel@webmail.astro.columbia.edu>
References: <558a57578e9fcefe5bd1400ff009cb05.squirrel@webmail.astro.columbia.edu>
Message-ID: <50EC1EF0.1090005@astro.columbia.edu>

Dear CBAers,

And now Gianluca Masi reports an ~80 minute signal from last night. 
This is now a very-high-priority morning target - for every conceivable 
hemisphere.

But forsake not T Pyx.  OT1126 may be just another prettier-than-normal 
normal dwarf nova (we dunno yet)...  but T Pyx has no equals!

joe




DEFINITELY an interesting target.  7 magnitudes is the magic number...
worth a special effort to nail for as long as possible!

joe



---------------------------- Original Message ----------------------------

--------------------------------------------------------------------------

OT J112619.4+084651 = Catalina transient

    CRTS detected a very large amplitude dwarf nova (>7 mag)
CSS130106:112619+084651.  The object is a very good candidate
for a WZ Sge-type dwarf nova.  Observations are encouraged.

SDSS magnitudes: 22.20, 21.83, 21.84, 22.28, 21.31
(no neural net solution for Porb, SDSS i mag may be too faint - eclipsing??)

    No previous outburst was detected in CRTS.

CSS130106:112619+084651
http://nesssi.cacr.caltech.edu/catalina/20130106/1301061090614105661.html
11 26 19.44 +08 46 51.0 14.84
http://skyserver.sdss3.org/dr8/en/tools/chart/navi.asp?ra=171.5809900&dec=8.7808300
CV



____________________________________________________________
Center for Backyard Astrophysics (CBA) mailing lists
https://cbastro.org/communications/mailing-lists/





From jop at astro.columbia.edu  Thu Jan 17 22:17:13 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Thu, 17 Jan 2013 22:17:13 -0500
Subject: (cba:news) Fwd: new stars for mid-January
In-Reply-To: <50F8AEA8.9050506@astro.columbia.edu>
References: <50F8AEA8.9050506@astro.columbia.edu>
Message-ID: <50F8BEB9.5070107@astro.columbia.edu>


Dear CBAers,

We finally reached critical mass on T Pyx.  I sent off an ATel
(#4743)which reported the new orbital period - kind of a shocker since
it implies a very large mass was ejected, inconsistent with the modern
understanding of recurrent novae.  Compared to Mario Livio's published
1991 prediction, the actual measurement is 7 times larger - and of the
opposite sign!  We can now take a little break from T Pyx.  We need to
pick it up again in March-April, to make sure the new period is truly
stable; it certainly oughta be, but T Pyx has surprised us at every turn...

BTW our journal paper on T Pyx (with all the authors, not just the few
in the ATel), supplying all the details behind this brief report and
trying to wrestle with understanding T Pyx in the context of binary
evolution, is about two weeks from a first draft.  The nova conference
in South Africa gives me a hard deadline.

At this exact moment in time, I recommend that very high priority be
given to:
(1) Nova Mon 2012: 06 39 38.57 +05 53 53.0, probably now about 13th mag.
The main period is 7 hours, so you'll want a LONG time series; 1-2
hours won't be useful.  We'll probably be observing this celebrity star
for many years - let's get acquainted with it!

(2) CSS130106:112619+084651 ("OT1126")  Let's ratchet up the pressure on 
this interesting WZ Sge type star.  Also will reward very long time 
series... but even the 2-hour variety will be useful.

And next tier of priority for

(3) ES Cet, DW Cnc, RX0704+26, Swift0732-13, HT Cam, CP Pup, V382 Vel 
(if it's still bright enough).  And V455 And, IF you can manage a cycle 
time of 15 s or less.

That still leaves the ER UMa stars for separate discussion.  The stars 
very thoroughly observed last year were ER UMa and BK Lyn; we don't need 
to make a big push this year, but we must spot-check them to make sure 
they don't go off the proverbial reservation (change their properties 
drastically).  I think that the major campaign on V1159 Ori is worth 
continuing 1 more week, and then stop; Enrique might want to countermand 
that, however.  We still haven't had much luck with RZ LMi, and that 
one's really quite a good target.

Most of the stars will reward faithfulness - staying with one star 
rather than one-night stands.  The exception is most DQ Hers.

For southerners who would like one star to stick with it for many weeks 
on end (I sure like data sets like that!), think about CP Pup.  It's 
time to figure out the periodic signals of this fascinating and 
incredibly elusive star!  RR Pic is another good choice; we haven't 
observed that one for years.
joe


From jop at astro.columbia.edu  Tue Jan 22 06:35:02 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Tue, 22 Jan 2013 06:35:02 -0500
Subject: (cba:news) LT Eri = SDSS J040714.78-064425.1
Message-ID: <50FE7966.6000404@astro.columbia.edu>

Dear CBAers,

We have an HST observation of this star coming up in a few days - make 
this star a very high (the highest) priority now.  *Both* for magnitude 
estimation (the imperative) and for a long time series, which will 
likely be quite interesting since it eclipses and has other periodic 
signals as well.

Late in the night, remember OT J122221.6-311525 - just discovered, still 
bright and humping, and likely to be an important star for years to come.

Nova Mon 2012 is also a definite keeper, and very important once the 
Moon gets out of the way.  But make SDSS 0407 your prime evening target. 
And don't spurn it because someone else is observing it; we need to be 
well calibrated on this star, and with HST soon jumping on it, we want 
to be solidly on the air before, during, and after the space observation.

joe


From jop at astro.columbia.edu  Mon Jan 28 19:43:43 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Mon, 28 Jan 2013 19:43:43 -0500
Subject: (cba:news) CP Puppis, mostly
Message-ID: <51071B3F.40406@astro.columbia.edu>

Dear CBAers,

There sure a lot of great stars out there for our purposes - OT1126+08, 
SSS1222-31, and Nova Mon 2012... all rather unusual - borderline 
mysterious - stars executing nice periodic signals.  Keep up the great work!

To my delight, Berto Monard and Bob Rea have taken me up on my 
suggestion of CP Pup.  Their data shows big periodic humps near 90 
minutes - but amazingly (to me) they just don't clearly define a period. 
  I've never seen anything quite like it.  Even if you fit the data with 
the most complicated thing I can easily imagine (roughly equal 
contributions from orbit, positive superhump, and negative superhump), 
it still doesn't fit.  Accretion disk weather!

The best way out of this is to get the densest possible light curve. 
There's a lot of water in the southern heminphere, so it won't be easy. 
  But if we could get South America (Arto?  Josch?) on this star, and 
also western Australia (Greg), we could nearly track it around the 
clock.  Jan-Feb is certainly CP Pup season.  Pretty please?

I'm suggesting holding your fire re T Pyx for a couple more weeks.  We 
definitely want another salvo of data from it later in the observing 
season (about a month hence), which will nicely constrain whether the 
new (post-outburst) period is evolving or constant.

No changes in the northern menu.  For those of you doing RX0704+26 = 
V418 Gem, I strongly recommend a *short* integration time, which you 
really need to properly resolve the strong 240 s pulse.  Most observers 
think they need to go long for this star - because it's faint (~17.4), 
and because the light curve *looks* very noisy.  But it's likely that 
most of what you see as noise is actually pulse amplitude (!)  So send 
me that noisy light curve - and if you take a power spectrum, you should 
see that 240 s signal easily.  (It's listed as 480 s, but apparently the 
star has two active poles, because nearly all the power is at 240).

joe


From jop at astro.columbia.edu  Tue Jan 29 18:24:06 2013
From: jop at astro.columbia.edu (Joe Patterson)
Date: Tue, 29 Jan 2013 18:24:06 -0500
Subject: (cba:news) Fwd: SDSS1005+1911
In-Reply-To: <CABkVZH0Q-KNebZOPe0=qgYijZuLXc0qbvUxcBtPhf-7D4GZ=9g@mail.gmail.com>
References: <CABkVZH0Q-KNebZOPe0=qgYijZuLXc0qbvUxcBtPhf-7D4GZ=9g@mail.gmail.com>
Message-ID: <51085A16.8000709@astro.columbia.edu>

Dear CBAers,

He means business!  Can you possibly observe this star *tonight*?  Just 
to remind, HST won't observe stars which might be in eruption, so we 
need observations right up to the date of observation (for permission to 
observe) and on the date (for maximum science impact).  It doesn't have 
to be a long time series, but make sure it's an actual magnitude - not 
just a differential magnitude (i.e. make sure you know the magnitude of 
the comparison star).

joe

oh, and send right away to Boris.



Subject: SDSS1005+1911
From: Boris Gaensicke <Boris.Gaensicke at warwick.ac.uk>
To: Joe Patterson <jop at astro.columbia.edu>
Content-Type: text/plain; charset="ISO-8859-1"
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Hi Joe,

can you send a note to your CBA army that we *urgently* need
some V-band measurements for SDSS1005+1911? It is
planned for tomorrow night, and we haven't had any
observation for the past 2 days, so I am getting a bit
anxious... more details are here

http://www.aavso.org/aavso-special-notice-329

Thanks!

Boris