From jop at astro.columbia.edu  Tue Jul  7 22:20:30 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Tue, 07 Jul 2015 22:20:30 -0400
Subject: (cba:news) Fwd: [vsnet-alert 18832] V380 Oph deep fading
In-Reply-To: <E1ZCeKC-0001tD-L4@ori.kusastro.kyoto-u.ac.jp>
References: <E1ZCeKC-0001tD-L4@ori.kusastro.kyoto-u.ac.jp>
Message-ID: <559C88EE.70808@astro.columbia.edu>

Oooooo, now there's a deep fading!  18.8 mag is kind of intimidating, 
maybe... but there's a decent chance the star has a very hefty 
sinusoidal signal with a period near 3.5 hours.  (That's one theory for 
what should happen in deep fadings.)

joe


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V380 Oph deep fading

   A similar deep fading was recorded in 2012.

   YYYYMMDD(UT)   mag  observer
   20150626.953  15.77CV  (Adolfo Darriba Martinez)
   20150627.023  16.83CV  (Adolfo Darriba Martinez)
   20150627.938  15.79CV  (Adolfo Darriba Martinez)
   20150704.070  18.81CV  (Adolfo Darriba Martinez)
   20150704.077  18.65CV  (Adolfo Darriba Martinez)
   20150704.083  18.78CV  (Adolfo Darriba Martinez)
   20150704.093  18.32CV  (Adolfo Darriba Martinez)
   20150704.105  18.36CV  (Adolfo Darriba Martinez)
   20150704.116  17.99CV  (Adolfo Darriba Martinez)
   20150704.127  18.44CV  (Adolfo Darriba Martinez)
   20150704.935  18.75CV  (Adolfo Darriba Martinez)
   20150704.947  19.02CV  (Adolfo Darriba Martinez)




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From jop at astro.columbia.edu  Wed Jul  8 22:38:43 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Wed, 08 Jul 2015 22:38:43 -0400
Subject: (cba:news) V339 Del and UX UMa
In-Reply-To: <559DDD14.9030408@centurytel.net>
References: <559B4226.1070303@astro.columbia.edu>
 <1647589828.1343648.1436362906514.JavaMail.yahoo@mail.yahoo.com>
 <559D2ED3.1080402@astro.columbia.edu>
 <7290917B-BB21-4C16-94E0-FABC69C6DA64@gmail.com>
 <559DB9B8.5000905@centurytel.net>
 <12D556DD-5BC3-4298-89AA-02BA0AE2D9AB@gmail.com>
 <559DDD14.9030408@centurytel.net>
Message-ID: <559DDEB3.8000103@astro.columbia.edu>

Yeah, V339 Del appears to be a loser.  Nice performance at other 
wavelengths, but pretty flat in the optical.  Time to quit at optical 
wavelengths.

And for that matter, time to quit on UX UMa (even for the diehards). 
The periodic signals continue to amaze, but the runs are getting too 
short, and it's time to move on.

IGR 1955+00 remains awfully interesting!  And some time series on V404 
Cygni would be mighty nice too.

joe


On 7/8/2015 10:31 PM, Jim Jones wrote:
> Enrique
>
> Then I won't bother making a run to link up with Davids.
>
> Jim
>
> On 7/8/2015 5:28 PM, Enrique de Miguel wrote:
>> Jim,
>>
>>   David is using V filter.
>> With the current data, no modulation comes up in the light curve.
>>
>> Enrique
>>
>> On Jul 9, 2015, at 2:00 AM, Jim Jones wrote:
>>
>>> What filter David?
>>>
>>> Jim Jones
>>>
>>> On 7/8/2015 4:21 PM, David Cejudo wrote:
>>>> I am actually following V338 Del as Enrique asked me to.
>>>> I may change targeta if neded, though.
>>>>
>>>> David Cejudo.
>>>>
>>>>
>>>>
>>>>
>>>>> El 8/7/2015, a las 16:08, Joe Patterson <jop at astro.columbia.edu>
>>>>> escribi?:
>>>>>
>>>>> Hi Donn et al.,
>>>>>
>>>>> Thanx for the details.  Yes, I think it is a "super-period" around
>>>>> 12 hours or so... but the precise value will depend on filter
>>>>> issues (since the AM Her stars often show really bright I emission
>>>>> due to cyclotron emission).  The basic period seems to be 81
>>>>> minutes, a very plausible Porb - but the star is pretty remarkable
>>>>> for its super-period, and for its huge variations on a timescale of
>>>>> just a few seconds (or maybe even less than 1 sec!).
>>>>>
>>>>> As Enrique says, we'll be able to splice these light curves
>>>>> together better when the star transits closer to local midnight.
>>>>> Shawn
>>>>> (easternmost USA observer) and Josch/Arto (Chile observers) will be
>>>>> in a good position to splice with Spanish observers (Enrique,
>>>>> David, Tomas).  And Gordon (AU) may be able to splice with Berto (ZA).
>>>>>
>>>>> joe
>>>>>
>>>>>> On 7/8/2015 9:41 AM, Donn Starkey wrote:
>>>>>> Joe, et.al.:
>>>>>>
>>>>>> My runs on IGR J19552+0044 were performed using a clear filter.  The
>>>>>> comp star was AAVSO 145 and the K star was AAVSO 148.  I used the R
>>>>>> magnitude for these two stars:
>>>>>>
>>>>>> C star    AAVSO 145     R mag 14.258
>>>>>> K star    AAVSO 148     R mag 14.292
>>>>>>
>>>>>> Exposure times were at 120 sec for each night of observation.
>>>>>>
>>>>>> Because of the placement of this star [or maybe because of my
>>>>>> placement
>>>>>> in relationship to the star] I started observing a very high air
>>>>>> masses.  Originally, I had thought that the star was brightening
>>>>>> during
>>>>>> the run due to lowering air masses, but subsequent runs shows that
>>>>>> the data did not appear to be effected by the air mass.  Is this a
>>>>>> long
>>>>>> term period fluctuation on the order of a multiple of ~12 hours?
>>>>>>
>>>>>> I am out of town until the 17th, but will continue observations on
>>>>>> this
>>>>>> target when I return home....unless directed otherwise.
>>>>>>
>>>>>> Donn
>>>>>>
>>>>>>
>>>>>> ----------------------------------------
>>>>>> Donn Starkey
>>>>>> donn at starkey.ws <mailto:donn at starkey.ws>
>>>>>>
>>>>>>
>>>>>>
>>>>>> ------------------------------------------------------------------------
>>>>>>
>>>>>>     *From:* Joe Patterson <jop at astro.columbia.edu>
>>>>>>     *To:* Gordon Myers <gordonmyers at hotmail.com>; Enrique de Miguel
>>>>>>     <edmiguel63 at gmail.com>; donn at starkey.ws
>>>>>>     *Sent:* Monday, July 6, 2015 11:06 PM
>>>>>>     *Subject:* IGR J19552+0044
>>>>>>
>>>>>>     Hi guys,
>>>>>>
>>>>>>     Helluva entertaining star this is!  The 81 minute period is very
>>>>>>     obvious, of course, and so are the super-fast (<5 s actually)
>>>>>>     oscillations in the "high state".  But I'm having trouble
>>>>>> putting these
>>>>>>     time-series on a common scale.  Because of the star's equatorial
>>>>>>     location, it's hard to get overlap - and we don't have any strict
>>>>>>     overlap.  In addition, there's some reason to believe that the
>>>>>>     brightness of the star is very different in V versus R versus
>>>>>> I. (Not
>>>>>>     known, but very possible.)
>>>>>>
>>>>>>     So can you state in detail how you derived your magnitudes
>>>>>> (even if you
>>>>>>     did in your original submission), and then copy all of us on
>>>>>> it?  I
>>>>>>     sure
>>>>>>     would like to figure out that longish period or quasi-period
>>>>>> that seems
>>>>>>     to be present (around a day?).
>>>>>>
>>>>>>     As you know, most CVs look pretty much the same at any
>>>>>> wavelengths near
>>>>>>     BVRI (their colors are usually close to B=V=R=I=0).  But the
>>>>>> magnetics
>>>>>>     (AM Hers) are often much brighter in I, because of cyclotron
>>>>>> radiation.
>>>>>>        You could perhaps check this by taking some data in I.
>>>>>>
>>>>>>     joe
>>>>> ____________________________________________________________
>>>>> Center for Backyard Astrophysics (CBA) mailing lists
>>>>> https://cbastro.org/communications/mailing-lists/
>>>> ____________________________________________________________
>>>> Center for Backyard Astrophysics (CBA) mailing lists
>>>> https://cbastro.org/communications/mailing-lists/
>>> ____________________________________________________________
>>> Center for Backyard Astrophysics (CBA) mailing lists
>>> https://cbastro.org/communications/mailing-lists/
>> ____________________________________________________________
>> Center for Backyard Astrophysics (CBA) mailing lists
>> https://cbastro.org/communications/mailing-lists/
>>
>
> ____________________________________________________________
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> https://cbastro.org/communications/mailing-lists/

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From jop at astro.columbia.edu  Thu Jul  9 15:09:28 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Thu, 09 Jul 2015 15:09:28 -0400
Subject: (cba:news) V380 Oph (fwd)
In-Reply-To: <alpine.DEB.2.10.1507091414450.29055@mira.aavso.org>
References: <alpine.DEB.2.10.1507091414450.29055@mira.aavso.org>
Message-ID: <559EC6E8.9080406@astro.columbia.edu>

Yes, this seems to be a *fresh* fading - so in theory, it's now a bare 
white dwarf and an orbiting M dwarf.  If the WD is hot (it should be), 
then the reflection effect off the M dwarf should produce a sinusoidal 
signal at Porb.  So the amplitude of the signal furnishes a bolometer 
for the WD.  It's an experiment we rarely get to do, because the 
accretion disk normally *shadows* the secondary from (most) WD light.

So it's a great target for time-series photometry.  Unfiltered is OK 
(perhaps necessary), but something redder (R?) might be better.

joe

On 7/9/2015 2:21 PM, Matthew Templeton wrote:
> Good afternoon Joe,
>
> I wanted to send a quick followup regarding V380 Oph.  Stella and I were
> talking this morning and are considering putting out a special notice on
> this star.  Do you have any thoughts or requests for what you'd like?
>
> I don't know that there are any multiwavelength followups or
> spectroscopy planned, but given that we don't have any data in the AAVSO
> database of this star at minimum, it would be good for posterity's sake
> if people are encouraged to get some data.  We currently have a little
> bit of data by Gordon Myers and Lew Cook from the past couple of days --
> the variations phase on the orbital period (0.154d) so they're doing a
> good job of detecting it.  The clear filter amplitude is about a
> magnitude, 19.3 to 18.8 for what looks like a sinusoid, with some bright
> deviations up to 18.4 or so.
>
> Let us know if you have any requests, otherwise Elizabeth Waagen and/or
> I will get something out Friday AM.
>
>      Matt
>
> Matthew Templeton, Ph.D.
> Science Director
> American Association of Variable Star Observers
> -----------------------------------------------
> Please support the AAVSO and its mission --
> Join or donate today: http://www.aavso.org/apps/donate
>
>
> ---------- Forwarded message ----------
> Date: Wed, 8 Jul 2015 10:31:32 -0400 (EDT)
> From: Matthew Templeton <matthewt at aavso.org>
> To: Joe Patterson <jop at astro.columbia.edu>
> Cc: eowaagen at aavso.org, sara at aavso.org
> Subject: V380 Oph
>
> Good morning Joe,
>
> I hope this email finds you well & enjoying summer.
>
> We received an email from Adolfo Darriba this morning about V380 Oph and
> he mentioned an Alert we sent out three years ago for an HST program on
> this.  As far as I've heard there isn't anything in the pipeline, but I
> wanted to check in case you need us to put something out -- we'll be
> happy to do so, just give us the typical details of what's needed when.
>
> Clear skies,
>
>      Matthew
>
> Matthew Templeton, Ph.D.
> Science Director
> American Association of Variable Star Observers
> -----------------------------------------------
> Please support the AAVSO and its mission --
> Join or donate today: http://www.aavso.org/apps/donate
>

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From jop at astro.columbia.edu  Thu Jul 16 15:55:23 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Thu, 16 Jul 2015 15:55:23 -0400
Subject: (cba:news) UX UMa, and IGR J1955+00
Message-ID: <55A80C2B.5070404@astro.columbia.edu>

Dear CBAers,

Some homework on these two stars!

UX UMa. I've drafted up a paper, minus the interpretation stuff, and 
with figures unlabelled and fragmentary (both attached), but I need some 
help from you.

1. Author list.  Can you check table 1 and supply, if you know it, how 
many nights/hours you contributed to this campaign.  Also, if possible 
and if consistent with some approximation to uniformity, tell me how 
you'd like your observatory/telescope described.  For actual authorship, 
I've usually used the criterion "at least 5% of the data", but since 
there are so many contributors, I might include everyone here.  For 
completeness you might also send your postal address, and if you like 
you can use your observatory name there, if you have one.

2. I was surprised, almost shocked, by the large-amplitude 3.7 day 
signal.  UX UMa has been very thoroughly studied for 60 years by some 
people (Walker, Krzeminski, Smak, etc.) who don't miss much.  They never 
had data like this, but I don't think they could have missed an effect 
this big.  Is the star unusually bright or faint this year?  It  would 
be nice if we knew!  Retroactively is fine.  If you have observed the 
star in this year's campaign, take some data exactly as you did and, 
more or less simultaneously, take some time series with calibrated V.

3.  And if you're so inclined, take another two weeks of time series, 
just to track this large-amplitude signal.

IGR J1955+00.  If you've observed this star, you know it's not like any 
other star we've ever discussed.  The 81 minute orbital (?) variations 
are huge, and the fast variations are huge and crazily fast.  We don't 
have the aperture and time resolution to explore the latter point... but 
the most likely interpretation at this point is that it's a radial 
accretor (AM Her star) and we're seeing cyclotron radiation from the 
accretion funnel.  That would imply an extremely red color for the 
variation - much redder than any (plausible) thermal process could 
manufacture.  We really need *simultaneous* time series in two colors - 
V and I would be an OK choice, and R and I would also be a good pair.
The more strictly simultaneous, the better.  Maybe you can use cba-chat 
to accomplish this: A does V, B does I, and we can thereby synthesize V-I.

Remarks on other stars tomorrow.

joe



(a)
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From jop at astro.columbia.edu  Wed Jul 22 17:24:43 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Wed, 22 Jul 2015 17:24:43 -0400
Subject: (cba:news) IGR J1955+00 and V1101 Aql
Message-ID: <55B00A1B.6090704@astro.columbia.edu>

Hi CBAers,

The data you've submitted on J1955 *does* show that the 81 minute 
periodic humps have very red colors, as we speculated/expected on the 
hypothesis that it's a magnetic CV (AM Her star).  Experiment done.

We don't need any more filtered data on it - you can go back to 
white-light observing and improve the time resolution.  Most of all, we 
need to splice the various time series, to establish a common 
instrumental scale.  For stars near the equator, oceans create a 
problem.  In particular, our Spanish observers should take the star 
pretty far into the west, and eastern USA observers (Shawn?) should pick 
it up as soon as possible in the east.  Now's the time, since it 
transits near local midnight.

There may be a signal vaguely near 0.7-1.1 c/d (in addition to the huge 
81 minute signal), and we'll really need a range of longitudes to nail 
this down.  Very good star for AU-NZ observers too, for the same reason.

Joe Ulowetz's coverage of V1101 Aql shows that the big ~4 hr superhump 
signal is back.  We'd like to cover at least over one dwarf-nova cycle 
(~16 d), to see if it's roughly the same thing we studied in 2013-4.

LS IV-08 is a nice bright UX UMa star, and some day may reward us.  But 
I think not this year.  Berto and Rolf Carstens have been observing it - 
not much variability, and no hint of periods.  Let's drop the star and 
move on.

joe p
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From jop at astro.columbia.edu  Mon Jul 27 13:45:05 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Mon, 27 Jul 2015 13:45:05 -0400
Subject: (cba:news) stars for late July
Message-ID: <55B66E21.7070603@astro.columbia.edu>

Dear CBAers,

Attached is the almost-final UX UMa paper.  I'll send the figures 
separately Wednesday.  I have most of the contact and observing-log info 
right now, but certainly not all - please correct me.  And UX UMa is off 
the menu for sure.

I still haven't decided re IGR J1955+00 - I think Enrique will send 
advice re that.  It certainly is fascinating - but we may have reached 
the limit of what we'll learn.  But maybe not...?  A few more nights is 
probably a good idea.

There are a few seasonally-appropriate stars where we have gathered 
almost enough data to complete our study - but not quite.  These are 
V1315 Aql, V380 Oph, and V1974 Cyg.  It would be great to amass about 2 
solid weeks of coverage on them.  Those are the stars I recommend now 
for lengthy coverage.

It's also a very good season for coverage of DQ Her stars (intermediate 
polars).  I especially recommend, V2306 Cyg, V2069 Cyg, RX1654-19, V1223 
Sgr, and IGR 1817-25.  As always, Koji Mukai's intermediate-polar 
website is a great reference for these stars:

http://asd.gsfc.nasa.gov/Koji.Mukai/iphome/iphome.html

As most of you know, the DQ Hers are good targets for the occasional 
night here and there - whereas the novalikes/old novae especially repay 
very frequent, tightly clustered observation.

Finally, here are some seasonally-appropriate easy targets: V Sge, FO 
Aqr, AO Psc (V1223 Sgr is borderline in this category too).  The goal 
for those guys is a *long*-term ephemeris, and they're bright - so 
they're very good targets for people getting started in this enterprise 
(or for people with few opportunities).

Good luck!

joe
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From jop at astro.columbia.edu  Thu Jul 30 06:06:01 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Thu, 30 Jul 2015 06:06:01 -0400
Subject: (cba:news) Mostly T Pyx, and GD 552
Message-ID: <55B9F709.8080401@astro.columbia.edu>


Dear CBAers,

I'm finishing up the formal paper on T Pyx, and wanted to get all the 
attributions, contact info, etc. down right.  I attach the ASP 
conference-proceeding paper of 2013-4.  The upcoming paper is an 
expanded version (conference proceedings always give you tight page 
limits).  See if your contact info is correct and current.

I also attach a (compact) log of observations.  Attached is one possible 
form.  Some published logs have great clutter (start times of each 
observation, accurate to 0.1 second); that alone could run 50 pages.  So 
I've prepared a log which contains the basic information, yet brief 
enough that readers will actually look at it.  But you might have a 
better idea, and there could be errors here, too.  You'll only spot the 
errors in accounting for your own work, but that will alert me so I can 
do some more digging and amend the table accordingly.

Other papers are forthcoming on IM Nor, V378 Peg, GD 552.  The first two 
are simpler since the campaigns were much shorter.  As for GD 552, it's 
back in the sky for us borealites, and since our network is much 
stronger now, I want to make one last try to get a PRECISE orbital 
period from our photometry.  It's near 0.0713 days, but we could improve 
the accuracy by 100x if we could find the signal (it's weak, though the 
star isn't particularly faint, at 16.6).  Anyway it's an excellent 
all-night target for northern observers, at least on decent nights. 
(It's the star labelled "Cep 1" in the Downes catalogue.  There's a 
contaminating star, which you might - or might not? - need to include.)

I'll send the full UX UMa draft to you on Monday, when I get back to the 
city.  (I'm spending the summer in the Catskill Mountains, which is why 
I can get a lot of writing done... but don't have all my toys with me)

Oh... and in answer to Joe U's query: *yes*, the UX UMa campaign is 
over.  Here comes the Sun/And I say it's all right...

joe p
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           TABLE 1 - SUMMARY LOG OF OBSERVATIONS

Year  Nights/hours Observers

1995-6   14/85     Patterson
1996-7    7/29     Patterson
1997-8    8/33     Kemp
1998-9    8/29     Kemp
1999-00   6/26     Kemp
2000-1    5/24     McCormick
2001-2    4/18     Kemp, McCormick
2002-3   19/71     Rea, Kemp, Monard, Allen, Richards
2003-4   10/39     Rea, Allen, Monard
2004-5    7/24     Rea, Monard, McCormick
2005-6   23/90     Allen, Rea, Monard, Christie,
                   Moorhouse, McCormick
2006-7   30/99     McCormick, Allen, Monard, Bolt
2007-8   18/74     Rea, Bolt
2008-9   15/62     Rea, Monard, McCormick, Bolt
2010-11   7/24     Rea, Myers (before eruption)
2011    102/400    Oksanen, Monard, Lowther, Dvorak, 
                   Bolt, Krajci, Hambsch (eruption)
2011-12  54/221    Oksanen, Monard, Hanbsch, Myers
2012-13  68/243    Oksanen, Monard, Nelson, Hambsch,
                   McCormick
2013-14  15/61     Monard, Nelson, Oksanen, Myers
2014-15  33/154    Myers, Oksanen, Monard, Dvorak

____________________________________________________

Kemp      1.0/0.9 m   La Serena, Chile (CTIO)
Oksanen    0.3 m      Atacama, Chile (Caisey
                      Harlingten Observatory)
Rea        0.35 m     Nelson, NZ
McCormick  0.35 m     Auckland, NZ
Monard     0.35 m     Klein-Karoo Observatory
Hambsch    0.35 m     Atacama, Chile (Caisey
                      Harlingten Observatory)
Allen      0.4 m      Nelson, NZ
Nelson                Melbourne, AU
Christie   0.4 m      Auckland, NZ
Bolt       0.35 m     Perth, AU
Dvorak     0.3 m      Orlando, FL (USA)
Patterson 1.0/0.75 m  CTIO/SAAO 
Myers      0.42 m     Siding Spring, AU
Richards              Melbourne, AU
Lowther
Krajci     0.35 m     Cloudcroft, NM (USA)
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From jop at astro.columbia.edu  Thu Jul 30 19:22:42 2015
From: jop at astro.columbia.edu (Joe Patterson)
Date: Thu, 30 Jul 2015 19:22:42 -0400
Subject: (cba:news) V1315 Aquilae
Message-ID: <55BAB1C2.8040207@astro.columbia.edu>

Hi CBAers,

   The last 3 nights, by Jim Jones and Orville Brettman, show that V1315 
is displaying strong superhumps again - the signals with period slightly 
shorter than Porb (which *defines* negative superhumps), PLUS the 
long-period (beat of Porb and Pnsh) wave which is allegedly the wobble 
period of the accretion disk.

   Outstanding!  And the reason to keep this campaign going (maybe with 
some AU-NZ coverage too, to get closer to global coverage?).  So, 
contrary to my earlier message, the top northern target now is not GD 
552, but V1315 Aql.

   Jim is using the 137 star (000-BKG-531, V-13.735) as a comparison, so 
that would be a good choice.  Orville is using AUID 000-BKG-529, so that 
might be good too.

joe

P.S. The 2004 and 2012 campaigns on V1315 Aql very likely also showed 
these signals.  The results were not as precise or as certain as we 
could accomplish this year, given the seasonal timing and the 
improvements in our network.  Maybe V1315, unlike the other "permanent" 
superhumpers, really does have permanent superhumps.
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