The MASTER team found a new RCB candidate:
This star appears to be unusual among R CrB variables, and may be one of the most interesting and important MASTER discoveries. After all, surveys are looking for flaring stars, and this one was the first fading star for 101 confirmed MASTER CVs (plus 26 possible CVs) and 101 SNe and PSNe!
The most important thing about TYC 2505-672-1 is its unusual location in the Milky Way. The generally adopted view is that RCB stars are concentrated to the galactic bulge and have absolute magnitudes MV=-4..-5. If you look at Fig. 1 in Tisserand et al., arXiv:1211.2475 (http://arxiv.org/abs/1211.2475), you will see that most RCBs are at low galactic latitudes. The only exception is R CrB itself which is at b=51. But R CrB has galactic longitude l=45 which makes it reside in the direction of galactic bulge. Yet, at Vmax=5.9 it is likely just a kiloparsec away (for the distance modulus m-M=10), and several hundred parsecs above the galactic plane. But if we take MV=-4.3 for TYC 2505-672-1 with its V=10.7, distance modulus m-M=15 will put it at 10 kpc from the Sun in almost opposite direction from the galactic center! As stated in our discovery ATel, galactic coordinates (l, b) for this new variable are (191.7, +51.3). 10 kpc*sin(51.3) makes it 7.8 kpc above the galactic plane, which is not just beyond the bulge - it's far in the outer halo of Milky Way! The galactic extinction is negligeable in this direction, which is also confirmed by rather moderate (for the red giant) J-K color index of 1.04 in 2MASS.
So, either this is not a true RCB star (which one then? something even more interesting?), or it will put an end to the long-time speculations about the bulge concentration of R CrB variables. Or we will have to reconsider the intrinsic magnitude scale for this type of (super)giants.
Good web pages say (and they don't lie) that RCB is a short phase in the evolution of a star. If there are ~100 stars of this type known in our own Galaxy, and RCB phase lasts for ~1000 years, there should be a new star every ~10 years entering this phase for the first time. It would be very interesting to know if the first fading episode (when there's no carbon dust around) is different from the next ones. For instance, the typical RCB variables which have already "been there, done that" are fading from the max to the min within 1 week to 1 month. TYC 2505-672-1, however, was likely constant at least during the last 60 years, and took more than 3 months to fade by ~4m. This also doesn't look like a typical RCB behavior. But, again, we may just have not enough statistics on the RCB fading episodes and the intervals between them.
We are still missing the spectrum of this variable. Actually, even the color was not measured! So, if you have RZ LMi in your CCD monitoring program, please consider changing the coordinates of your telescope's pointing center to someting like 09 52 30 +34 00 10! Of course, if your field of view is larger than 15'x15' - there's 21.5' between the two variables. The star is added to AAVSO VSX with AUID 000-BKW-029, see http://www.aavso.org/vsx/index.php?view=detail.top&oid=297394.
"The object's behavior is unusual for the typical R CrB stars. This may be the first active episode of the red giant entering the short RCB phase. That may explain the absence of surrounding carbon dust, small J-K colors and presence of hydrogen emission. We encourage the continued spectroscopic and photometric monitoring to follow up the evolution of the current fading episode."
More info: http://www.astronomerstelegram.org/?read=4834
I think it is very unlikely that the interpretation in,
is correct. As far as we know, hydrogen-rich red giants do not evolve to become hydrogen-deficient RCB stars.
I don't know, but the star has not been listed in Tisserand's RCB candidates: Tracking down R Coronae Borealis stars from their mid-infrared WISE colours.
I wonder what kind of object is this star? Any spectrum availabe?
There is a spectrum here: http://www.astronomerstelegram.org/?read=4834.
I suspect it is a rather unusual eclipsing binary.
I could glimpse this intriguing star last night and estimated it at mag. 15.1. It looks like it is getting slowly brighter?
(60days - lightcurve)
The spectrum illustrated is consistent with the published M2III, with the addition of weak H-alpha emission. The JHK colours are also consistent with this. This is rather an early type for a semiregular variable, especially as it is well below maximum light - much of the light drop in red variables of spectral type M results from the increasing strength of the TiO bands, which define the spectral subtype, as the star approaches minimum. It could however be a metal poor star with intrinsically weak bands. An interesting alternative is that it is an M star which has produced a dust cloud. This is well established for carbon stars (not just RCB but also regular SR and Mira types). This has been seen in an SC star, UY Cen, so maybe it can also occur in an M star of less or no C enrichment.
The most useful observation which could be made now, in addition to continued monitoring, is to re-observe the JHK colours. If it has ejected dust in the line of sight, it should have become substantially redder than appropriate for the spectral type, possibly with an IR excess. The latter would be best seen at L, but might show at K.
I am also increasingly of the belief that this object is not a true R CrB-type star. Depending on just how you view the error brackets of the CCD data, it seems to me that the star has probably been very nearly constant since it reached the bottom of its initial decline many months ago. Anyone know of any further announcements, or articles, addressing it that might better define the true nature of this star?
I made my first observation this season: It looks like it's slowly rising!
I've taken my first obs of TYC 2505-672-1 and it does seem to be brighter than previous estimates.
Nicely placed for a few months of scrutiny.
still rising! Yesterday i estimated it at mag. 13.5
Do we already know what kind of object this is? It's still a RCB: in VSX.
As far as we can tell, it is not an RCB star. It could be a Mira making dust. My colleague, Patrick Tisserand, looked at the IR colors and it doesn't look like an RCB star. Also, Pickles et al. (2010) http://cdsarc.u-strasbg.fr/viz-bin/Cat?VI/135 suggests that it is an M2 III star from its visible colors. It would be great if someone got a spectrum of this star so we can see what it really is.
It might be a very long period eclipsing binary, similar to V1381 Sco (A8II+M5Ia; per= 6545 d.) and V1383 Sco (F0Ib+M1-M7/8I; per= 4876 d.).
The eclipse amplitudes of these supergiant systems are very large.
I wouldn't trust Pickles spectral types. I've seen a lot of reddened early types classified as M giants.
Observations during the recovery phase to see if the rising and descending branchs are symmetric would be helpful too.
That faint CRTS datapoint before the deep eclipse conspired against the EA classification but it could only be a wrong observation (however, the error figure is similar to the rest of the observations).
I find it interesting that although the current rise toward maximum light seems to be very protracted, nevertheless it looks to have been very nearly (precisely?) linear in nature. I would note also that at the star's current rate of brightening it looks like the full recovery process will require close to 12 months in total. This certainly smacks of the egress from some sort of stellar eclipse event, at least to me.
Wouldn't ya just know it! I no soon posted my impression that this star's recovery appeared to be almost perfectly linear and it probably was no more than a simple eclipsing binary of very long period when my next observation, taken on Februrary 26/27, indicated an abrupt DROP of several tenths of a magnitude in its brightness. Perhaps there is something stranger about the exact nature of this variable after all. Might it still be a long period Algol-type system, but with an obscuring cloud/disk surrounding the eclipsing component? Hmmm.
So we need more observations now to see how far this new fading goes and it would be nice if more people start paying attention to this one!
I too, find John's most recent observation very interesting ! I have added in a Vmag result obtained a couple of nights ago (before the fade) which supports the evidence that we've had a slow steady rise underway for awhile now. As luck would sometimes have it, I had planned to observe this star again before dawn this morning but the field had dropped below the 'scopes' lower alt limit by the time I was ready to go. I shall try again tonight (earlier this time!).
I'm sure our former AAVSO Circular editor will remember past cases like EE Cep and HBV 483, both suspected as possible RCBs back in the day and both having their true natures come to light after further study, including spectra.
The apparent minor dimming noted by BRJ several nights back has evidently not persisted. Observations made a few hours ago suggest the relatively slow brightening trend we've been witnessing over the past few weeks and months has probably resumed.
I read it would be nice to have a recent spectrum, so I asked if someone on the dutch forum "astroforum.nl" could take one from such a faint star.
Paul Gerlach took up the challenge. He normalized it at 4700 Å and adjusted the intensity so that it could be compared to the spectrum from 2013.
Can something be deduced from it? Is this a usefull observation? I don't know anything about spectroscopy, so any comment would be nice!
(EDIT: the most important part (with H-alfa) on the right is not visible. But you can view it with right-click)
Well it's still on the rise, I measured it last night at 12.697.
Interestingly enough, it looks to me that this star's behavior mid-February through the very beginnings of March was some manner of slow brightness "hiccup". But by the second week of March the lightcurve appears to my eyes basically to have returned to the line and rate of brightening exhibited in its former brightening trend. Odd behavior, indeed.
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