Showing posts with label variable stars. Show all posts
Showing posts with label variable stars. Show all posts
Wednesday, December 9, 2015
Variable Star workshop on KIC 8462852 at VSSEC
Friday, November 4, 2011
FS Aur is back!
Well, that highly erratic variable cataclysmic variable star FS Aurigae (FS Aur) is back in season and has not disappointed so far with two great outbursts already.
The quiescent duration between outbursts does seem a bit longer than the previous season - so far, but as we saw in the last northern winter, it was prone to springing a few surprises.
More on this soon, Vitaly has a nice slide deck now which he presented at a conference recently.
Regards
Peter
Sunday, March 13, 2011
FS Aur Video
As you all know I have been helping Dr Vitaly Neustroev with his research on FS Aur. This is a very erratic variable star that can vary in magnitude by up to 0.2m over an hour, has a number of interacting periodic cycles, and goes into outburst every 13-15 days.
Whilst this video doesn’t really do justice to all the hardwork and the more subtle variations, it none the less is a bit of fun to show you what we have been looking at.
The timescale is a very rough 1 sec = ~2 days.
Enjoy!!!!
Astroswanny
Whilst this video doesn’t really do justice to all the hardwork and the more subtle variations, it none the less is a bit of fun to show you what we have been looking at.
The timescale is a very rough 1 sec = ~2 days.
Enjoy!!!!
Astroswanny
Sunday, March 7, 2010
GW Lib data to support Hubble COS mission
One of the delights of being an amateur astronomer is being able to assist real scientists with (hopefully) useful data on various targets that they need to keep an eye on prior to observation runs with toys that I can't afford eg the HST.
An alert (Notice#417) went out this week from the AAVSO requesting data on two cataclysmic variable stars to support Dr Paula Szkody's upcoming spectrograph observations on the Cosmic Origins spectrograph on the HST.
GW Lib is a CV that needs to be fainter than Mag 14 when the mission takes place, and it has been known to infrequently outburst.
AAVSO members regularly fly cover and give early warnings on any unexpected events that may affect the mission integrity.
GW Lib is at DEC -25.00.25 so that immediately eliminates a good number of the world's telescopes. Australia has had large monsoonal lows pushing into the interior of Australia and the weather has been pretty ordinary this week as a result.
My choice of a couple of 300 sec images was a little short in duration as the SNR was a bit low with the moon still being at 55%. I was able to confirm that the target was about Mag 15.39 (given the low SNR maybe a little closer to 16) in the Johnson V filter (untransformed).
I'll try again tonight with a little longer exposure.
Peter
UPDATE: 10/03/2010
JD Airmass GW_Lib 147 143 Err SNR
2455265.209 1.11373 15.501 14.422 14.000 0.025 42
2455265.214 1.100 15.421 14.432 13.988 0.031 34
2455265.219 1.08756 15.514 14.422 14.003 0.041 26
Ave 15.479 14.425 13.997 0.032 34
Peter
UPDATE: 11/03/2010
Today I tidied up my Sequence a little, deleting 128 and I added 157 to the comp star list as visually it looked to be the identical magnitude to GW Lib. I also stacked the three images with a median combine to give a much much stronger SNR. With the SNR of a number of the comp stars now being over 100 (preferred) the Magnitude of 147 was almost identical to the chart magnitude listed in AAVSO chart 2084CCS. Comfortable with the improvement in accuracy GW Lib magnitude was measured at 15.629 (Johnson V untransformed).
Note the stronger SNR of the target now at 60 with the comp star's SNR >100.
Seven AAVSO members contributed observations and Dr Paula was pleased to hand the observations to the Hubble space controllers this morning who then gave the go-ahead for tonights UV run on the Cosmic Origins spectrograph.
Congrats to Dr Paula, hope everything goes well tonight! It all starts again on the 14th as the next COS run is on V842 Cen.
An alert (Notice#417) went out this week from the AAVSO requesting data on two cataclysmic variable stars to support Dr Paula Szkody's upcoming spectrograph observations on the Cosmic Origins spectrograph on the HST.
GW Lib is a CV that needs to be fainter than Mag 14 when the mission takes place, and it has been known to infrequently outburst.
AAVSO members regularly fly cover and give early warnings on any unexpected events that may affect the mission integrity.
GW Lib is at DEC -25.00.25 so that immediately eliminates a good number of the world's telescopes. Australia has had large monsoonal lows pushing into the interior of Australia and the weather has been pretty ordinary this week as a result.
My choice of a couple of 300 sec images was a little short in duration as the SNR was a bit low with the moon still being at 55%. I was able to confirm that the target was about Mag 15.39 (given the low SNR maybe a little closer to 16) in the Johnson V filter (untransformed).
I'll try again tonight with a little longer exposure.
Peter
UPDATE: 10/03/2010
JD Airmass GW_Lib 147 143 Err SNR
2455265.209 1.11373 15.501 14.422 14.000 0.025 42
2455265.214 1.100 15.421 14.432 13.988 0.031 34
2455265.219 1.08756 15.514 14.422 14.003 0.041 26
Ave 15.479 14.425 13.997 0.032 34
Peter
UPDATE: 11/03/2010
Today I tidied up my Sequence a little, deleting 128 and I added 157 to the comp star list as visually it looked to be the identical magnitude to GW Lib. I also stacked the three images with a median combine to give a much much stronger SNR. With the SNR of a number of the comp stars now being over 100 (preferred) the Magnitude of 147 was almost identical to the chart magnitude listed in AAVSO chart 2084CCS. Comfortable with the improvement in accuracy GW Lib magnitude was measured at 15.629 (Johnson V untransformed).
Note the stronger SNR of the target now at 60 with the comp star's SNR >100.
Seven AAVSO members contributed observations and Dr Paula was pleased to hand the observations to the Hubble space controllers this morning who then gave the go-ahead for tonights UV run on the Cosmic Origins spectrograph.
Congrats to Dr Paula, hope everything goes well tonight! It all starts again on the 14th as the next COS run is on V842 Cen.
Wednesday, October 7, 2009
Variable stars and the discovery process
The weather has been kind this week allowing a return to varibale star observations. This week I will take a look at the discovery process for new variable stars, as this week I had reason to understand and work through it due to detecting what appears to be a new variable star that has not been previously listed.
Discoveries of variable stars are normally a specific targeted activity, from either a target list of suspected variables in a particular constellation, or by star type researching the characteristics of the variables. Teams of astronomers usually collaborate over many observing sessions to gather data and write up their findings in a science paper that is then published in one of the journals. One such paper was published only this week by Alex Golovin, Kirill Sokolovsky, Natalia Virnina, Javier Lopez Santiago - Three new Variable stars in Indus. The purpose of such papers is to provide data, classification information, star temperatures, period of variability, and assist scientists understand the behaviour, age and characteristics of these stars.
In 1844 the german astronomer Friedrich Wilhelm August Argelander appealed, "I lay these hitherto sorely neglected 30 variable stars most pressingly on the heart of all lovers of the starry heavens" spawning the study of variable stars by professionals and amateurs alike. Over the past 160 years years the list has grown north of 30,000 with another 15000 suspected of being variable. Due to the massive number of variable stars and the limited number of observers, alas many still remain neglected.
Today we know there are two types of variable stars (and I don't mean one of those amusing bumper stickers - those that are and those that aren't). The two types are intrinsic and extrinsic - ie variability within the star and variablily external to the star. The stars then fall into a number of classifications related to the behaviour within these two types.
Observation and studies of variable stars are directed at identifying the characteristics to determine these classifications, and then determine the behaviours of these stars in order to better understand the context of the stars lifecycle.
The Hertzsprung-Russell diagram is the current collective knowlege of stellar lifecycles, individual star types are referenced here but things get more complicated when some of these stars (of different types) orbit around each other and start interacting and exchanging their elements and debris. This can lead to very sudden changes in brightness and evidence of a catalysmic variable. [This is one example of an extrinsic variable. - EDIT Actually whilst that might sound like extrinsic behaviour its still intrinsic as in the case of Dwarf Nova the accretion disk collapses onto the star and then its brightness changes intrinsicly - Thanks Sebastion]
Image courtesy of CSIRO ATF Outreach
Anyway, I am starting to sound as about exciting as a live video broadcast of the visible debris cloud in the LCROSS impact......so I'll return to my story.
One other way discoveries are made is when observers are participating in an observering campaign, and whilst processing data they find something and say ..... "hang on what going on over here". Many discoveries in all disciplines of astronomy are made when you find something a little unexpected whilst observing something else. Even amateur astronomers become curious and just have to know why!!!
This week I found myself in such a situation. Using the great photometrica tool (the poster child for "astronomy cloud services" ie photometric analysis as a webservice) I was processing data on V4743 Sgr a Cataclysmic Variable that last went into outburst in 2002. When I had finished, I hit the "what else is varying in this field" button and was presented with a list of about 40 stars to inspect. I knocked out all the stars that had a double star in the annulus, knocked out all those with a SNR less than 100 and bingo I had three left. All had brightness changes that were much larger than the standard deviation of their comparison stars (first point of interest) and demanded closer inspection. One of those had a small asteroid/or hot pixel drifting past through the annulus and across the sky background....AHHH!!! more stuff to check...... (second point to always check for transient artifacts/objects). Back to my top candidate, a Mag 14 Star, I could see a clear straight line variation of about 0.4 magnitude in just 30 minutes of imaging time (third point of interest), I quickly reviewed some other data of the same field and reprocessed all the data in a different software program - Maxim DL, and bingo! (fourth point of interest....got the same result).
So like any good AAVSO member.....contact your mentor and say "What do I do now"?
The reporting of a variable star discovery is an interesting process, one I was about to learn. Whilst an exciting event for the observer and very satisfying, its not one that leads to Hubble time and NASA press conferences. None-the-less it is scientifically interesting.
The International Variable Star Index is the body that administers this process. There is an 11 step process to enter the data required: Position, all known identifiers in the various star catalogs (2MASS & UCAC3 etc), the magnitude, the amount of variability (Max/Min Mag), variable star type, the period of its variablility, a light curve and a phase diagram. The final data point is any published jounals listing research data on your discovery(example as per Golovin, Sokolovsky, Virnina, Santiago mentioned above).
If you make a report to the variable star index all this information is vital, as to have your discovery reported and confirmed it needs to be varifiable by others, and available for peer review.....thus the onus is on the discoverer to present the data that needs to be reviewed. Over the next couple of nights I collected additional data and prepared my submission. As this was the first time I had been through the process, and being very much in the AMATEUR Astronomy camp, I was very nervous about the process. Its always important to follow the process and accept the feedback that comes from those with much more experience than one's self.
I received back a very helpful email that rejected my submission (for now) due to the fact that I didn't have enough data to produce a full phase diagram and I had suggested that it may be a Cephid Variable due to the short period and hadn't considered that it was a bit too blue to be a Cephid and that it was more likely a RR-AB. The VSX person made some very helpful suggestions about what I should do next - get some more data and produce a full phase diagram and re-submit.
As you can see from my light curve there is nowhere near enough data to create a phase diagram, as my observing runs were of short duration.
So nothing to report yet, other than there is a little variable out there throbbing away with a period of a couple of hours and varying by about 0.9M just waiting for my next visit. Once I have the period length I can then re-submit and rally some other observers for follow up. Again, the most important learning has been that the the period is important as others need to know what to look for, so they can plan their observing campaign.
So in the spirit of Argelander's appeal, at 9pm tonight, I will return and ensure my little variable doesn't end up on a list of "hitherto sorely neglected" variable stars.
UPDATE: 16/10
Still chasing data, missed a couple of nights due to bad weather and now my little star is escaping into the western sky. Here is the Phase Plot I referred to....as you can see this is still a bit out and I need a lot more data. At least you can see what I need here, to calculate the period.
Clear Skies!!
Discoveries of variable stars are normally a specific targeted activity, from either a target list of suspected variables in a particular constellation, or by star type researching the characteristics of the variables. Teams of astronomers usually collaborate over many observing sessions to gather data and write up their findings in a science paper that is then published in one of the journals. One such paper was published only this week by Alex Golovin, Kirill Sokolovsky, Natalia Virnina, Javier Lopez Santiago - Three new Variable stars in Indus. The purpose of such papers is to provide data, classification information, star temperatures, period of variability, and assist scientists understand the behaviour, age and characteristics of these stars.
In 1844 the german astronomer Friedrich Wilhelm August Argelander appealed, "I lay these hitherto sorely neglected 30 variable stars most pressingly on the heart of all lovers of the starry heavens" spawning the study of variable stars by professionals and amateurs alike. Over the past 160 years years the list has grown north of 30,000 with another 15000 suspected of being variable. Due to the massive number of variable stars and the limited number of observers, alas many still remain neglected.
Today we know there are two types of variable stars (and I don't mean one of those amusing bumper stickers - those that are and those that aren't). The two types are intrinsic and extrinsic - ie variability within the star and variablily external to the star. The stars then fall into a number of classifications related to the behaviour within these two types.
Observation and studies of variable stars are directed at identifying the characteristics to determine these classifications, and then determine the behaviours of these stars in order to better understand the context of the stars lifecycle.
The Hertzsprung-Russell diagram is the current collective knowlege of stellar lifecycles, individual star types are referenced here but things get more complicated when some of these stars (of different types) orbit around each other and start interacting and exchanging their elements and debris. This can lead to very sudden changes in brightness and evidence of a catalysmic variable. [This is one example of an extrinsic variable. - EDIT Actually whilst that might sound like extrinsic behaviour its still intrinsic as in the case of Dwarf Nova the accretion disk collapses onto the star and then its brightness changes intrinsicly - Thanks Sebastion]
Image courtesy of CSIRO ATF Outreach
Anyway, I am starting to sound as about exciting as a live video broadcast of the visible debris cloud in the LCROSS impact......so I'll return to my story.
One other way discoveries are made is when observers are participating in an observering campaign, and whilst processing data they find something and say ..... "hang on what going on over here". Many discoveries in all disciplines of astronomy are made when you find something a little unexpected whilst observing something else. Even amateur astronomers become curious and just have to know why!!!
This week I found myself in such a situation. Using the great photometrica tool (the poster child for "astronomy cloud services" ie photometric analysis as a webservice) I was processing data on V4743 Sgr a Cataclysmic Variable that last went into outburst in 2002. When I had finished, I hit the "what else is varying in this field" button and was presented with a list of about 40 stars to inspect. I knocked out all the stars that had a double star in the annulus, knocked out all those with a SNR less than 100 and bingo I had three left. All had brightness changes that were much larger than the standard deviation of their comparison stars (first point of interest) and demanded closer inspection. One of those had a small asteroid/or hot pixel drifting past through the annulus and across the sky background....AHHH!!! more stuff to check...... (second point to always check for transient artifacts/objects). Back to my top candidate, a Mag 14 Star, I could see a clear straight line variation of about 0.4 magnitude in just 30 minutes of imaging time (third point of interest), I quickly reviewed some other data of the same field and reprocessed all the data in a different software program - Maxim DL, and bingo! (fourth point of interest....got the same result).
So like any good AAVSO member.....contact your mentor and say "What do I do now"?
The reporting of a variable star discovery is an interesting process, one I was about to learn. Whilst an exciting event for the observer and very satisfying, its not one that leads to Hubble time and NASA press conferences. None-the-less it is scientifically interesting.
The International Variable Star Index is the body that administers this process. There is an 11 step process to enter the data required: Position, all known identifiers in the various star catalogs (2MASS & UCAC3 etc), the magnitude, the amount of variability (Max/Min Mag), variable star type, the period of its variablility, a light curve and a phase diagram. The final data point is any published jounals listing research data on your discovery(example as per Golovin, Sokolovsky, Virnina, Santiago mentioned above).
If you make a report to the variable star index all this information is vital, as to have your discovery reported and confirmed it needs to be varifiable by others, and available for peer review.....thus the onus is on the discoverer to present the data that needs to be reviewed. Over the next couple of nights I collected additional data and prepared my submission. As this was the first time I had been through the process, and being very much in the AMATEUR Astronomy camp, I was very nervous about the process. Its always important to follow the process and accept the feedback that comes from those with much more experience than one's self.
I received back a very helpful email that rejected my submission (for now) due to the fact that I didn't have enough data to produce a full phase diagram and I had suggested that it may be a Cephid Variable due to the short period and hadn't considered that it was a bit too blue to be a Cephid and that it was more likely a RR-AB. The VSX person made some very helpful suggestions about what I should do next - get some more data and produce a full phase diagram and re-submit.
As you can see from my light curve there is nowhere near enough data to create a phase diagram, as my observing runs were of short duration.
So nothing to report yet, other than there is a little variable out there throbbing away with a period of a couple of hours and varying by about 0.9M just waiting for my next visit. Once I have the period length I can then re-submit and rally some other observers for follow up. Again, the most important learning has been that the the period is important as others need to know what to look for, so they can plan their observing campaign.
So in the spirit of Argelander's appeal, at 9pm tonight, I will return and ensure my little variable doesn't end up on a list of "hitherto sorely neglected" variable stars.
UPDATE: 16/10
Still chasing data, missed a couple of nights due to bad weather and now my little star is escaping into the western sky. Here is the Phase Plot I referred to....as you can see this is still a bit out and I need a lot more data. At least you can see what I need here, to calculate the period.
Clear Skies!!
Saturday, September 26, 2009
When you wish upon a star
Welcome. This week has been characterised by some fairly average weather. Those of you tuning into Australia's premier football event around the world this afternoon will see plenty of our famous Melbourne weather on show.
Weather can have an impact on an observing campaign, so there have been some challenges in obtaining some of the data I have been chasing this week. I am getting great positive feedback on the blog - largely because I am blogging on my observations.
So this week, given the weather, I thought it would be good to talk about observation campaigns. This week I have barely jagged a couple of short sessions on
V4743 SGR and some of the surrounding variables in the same field. V4743 Sgr is also referred to as Nova Sgr 2002c making it an object of some interest, given its nova outburst in 2002. Over 200 observers have contributed to the AAVSOs lightcurve.
So what is it that makes an object "interesting"? Clearly a Nova outburst is something that is interesting, as professional astronomers are quick to follow up with highly accurate spectroscopy. The advantage of having amateurs "on their toes" and participating in regular campaigns is that professional astronomers can't afford to have billion dollar telescopes pointed at stars, waiting for years, for something to happen. (The hubble deep field shot is a noteable exception...but a deliberate experiment to look at nothing to see if something WAS there)
A good example of leveraging the skills of amateur astronomers is my data here on QU Sgr. This is a Mira variable star of little or no interest to anyone.....but who knows one day it may be significant or do something. If that ever happened, what would we have to compare it with? So whilst gathering some data on V4743 with my set up which has a fairly large field of view, it is important to grab a couple of readings on any other Variables in the field, as other observers are unlikely to ever go specifically to QU Sgr to collect data.
There are a plethora of variable stars requiring regular observations and a limited number of observers. Today we have the fantastic use of social networking, blogs, forums and membership of organisations such as AAVSO. In this environment connected communities of dedicated amateurs have organised campaigns based on a prioritised list of "interesting objects".
Rod Stubbing who discovered this months outburst of VX For was working through a carefully targeted list of variables that were "in season" ie at an optimal position in the sky for observing. Rod indicated to me it was his first observing session on VX For for the year. So you never know what you will find, and how many other people who are observing.
So I leave you this week with the completely insignificant Mira Variable QU Sgr that noone else has reported on for over 4000 days.
Weather can have an impact on an observing campaign, so there have been some challenges in obtaining some of the data I have been chasing this week. I am getting great positive feedback on the blog - largely because I am blogging on my observations.
So this week, given the weather, I thought it would be good to talk about observation campaigns. This week I have barely jagged a couple of short sessions on
V4743 SGR and some of the surrounding variables in the same field. V4743 Sgr is also referred to as Nova Sgr 2002c making it an object of some interest, given its nova outburst in 2002. Over 200 observers have contributed to the AAVSOs lightcurve.
So what is it that makes an object "interesting"? Clearly a Nova outburst is something that is interesting, as professional astronomers are quick to follow up with highly accurate spectroscopy. The advantage of having amateurs "on their toes" and participating in regular campaigns is that professional astronomers can't afford to have billion dollar telescopes pointed at stars, waiting for years, for something to happen. (The hubble deep field shot is a noteable exception...but a deliberate experiment to look at nothing to see if something WAS there)
A good example of leveraging the skills of amateur astronomers is my data here on QU Sgr. This is a Mira variable star of little or no interest to anyone.....but who knows one day it may be significant or do something. If that ever happened, what would we have to compare it with? So whilst gathering some data on V4743 with my set up which has a fairly large field of view, it is important to grab a couple of readings on any other Variables in the field, as other observers are unlikely to ever go specifically to QU Sgr to collect data.
There are a plethora of variable stars requiring regular observations and a limited number of observers. Today we have the fantastic use of social networking, blogs, forums and membership of organisations such as AAVSO. In this environment connected communities of dedicated amateurs have organised campaigns based on a prioritised list of "interesting objects".
Rod Stubbing who discovered this months outburst of VX For was working through a carefully targeted list of variables that were "in season" ie at an optimal position in the sky for observing. Rod indicated to me it was his first observing session on VX For for the year. So you never know what you will find, and how many other people who are observing.
So I leave you this week with the completely insignificant Mira Variable QU Sgr that noone else has reported on for over 4000 days.
Wednesday, September 16, 2009
VX For Dwarf Nova Outburst .....update#2
The variable Star community is alive with excitement after Rod Stubbing an amateur astromomer from Victoria Australia discovered VX For in outburst for the first time since 1990.
After a 19 year spell the Dwarf Nova has moved into outburst. Importantly Rod appears to have caught it before its previous peak of 12.5 in 1990.
I was able to get some photometery on VX For and reported confirming data on Rod's exciting find to the AAVSO.
Mike Simonsen has written an excellent blog on this star with some of the history and the significance of the event. I imagine professional astronomers will be keen to get some spectroscopy on this interesting star in over the next month.
My observations were just a short run last night as the window is fairly tight from about 11:30Pm local time through to about 4:30am. The co-ordinates also restrict viewing to southern observers: RA 03:26:46.9 Dec -34:26:37.0 so our northern friends will have to leverage any access they can get to southern hemiphere scope......its called teamwork! Also Joe at the Center for Backyard Astrophysics is following the story with interest and rallying the troops!
Anyway it promises to be an exciting time as VX For entertains us for the coming weeks. My first light curve showed it right on the 13.0 magnitude observed the previous night by Rod Stubbing. Amateur Observers can post their results to the AAVSO.
Enjoy! I will post any further updates, you can also follow the light curve here as it develops.
After a 19 year spell the Dwarf Nova has moved into outburst. Importantly Rod appears to have caught it before its previous peak of 12.5 in 1990.
I was able to get some photometery on VX For and reported confirming data on Rod's exciting find to the AAVSO.
Mike Simonsen has written an excellent blog on this star with some of the history and the significance of the event. I imagine professional astronomers will be keen to get some spectroscopy on this interesting star in over the next month.
My observations were just a short run last night as the window is fairly tight from about 11:30Pm local time through to about 4:30am. The co-ordinates also restrict viewing to southern observers: RA 03:26:46.9 Dec -34:26:37.0 so our northern friends will have to leverage any access they can get to southern hemiphere scope......its called teamwork! Also Joe at the Center for Backyard Astrophysics is following the story with interest and rallying the troops!
Anyway it promises to be an exciting time as VX For entertains us for the coming weeks. My first light curve showed it right on the 13.0 magnitude observed the previous night by Rod Stubbing. Amateur Observers can post their results to the AAVSO.
Enjoy! I will post any further updates, you can also follow the light curve here as it develops.
Vx For Dwarf Nova outburst
Great work last night Rod. I jumped on it as soon as it came over the side of the shed and have it in the first image at an average of 12.951 M across the first three images I have downloaded (airmass of 1.5)
I should be able to tighten that up a bit when I process the rest of the run.
Data from my first image....
VX For 12.951 SNR 103
126 12.555 SNR 137
137 13.652 SNR 59
More later....
Firrst three images down:
#TYPE=EXTENDED
#OBSCODE=LPB
#SOFTWARE=Photometrica 3.0
#DELIM=,
#DATE=JD
#NAME,DATE,MAG,MERR,FILT,TRANS,MTYPE,CNAME,CMAG,KNAME,KMAG,AMASS,GROUP,CHART,NOTES
VX For,2455090.09733,12.936,0.011,V,NO,ABS,ENSEMBLE,na,137,13.660,1.55703,na,090915,na
VX For,2455090.09994,12.959,0.010,V,NO,ABS,ENSEMBLE,na,137,13.665,1.53358,na,090915,na
VX For,2455090.10256,12.991,0.011,V,NO,ABS,ENSEMBLE,na,137,13.662,1.51102,na,090915,na
Looks like Rod has bagged a beauty!!!!
Peter
I should be able to tighten that up a bit when I process the rest of the run.
Data from my first image....
VX For 12.951 SNR 103
126 12.555 SNR 137
137 13.652 SNR 59
More later....
Firrst three images down:
#TYPE=EXTENDED
#OBSCODE=LPB
#SOFTWARE=Photometrica 3.0
#DELIM=,
#DATE=JD
#NAME,DATE,MAG,MERR,FILT,TRANS,MTYPE,CNAME,CMAG,KNAME,KMAG,AMASS,GROUP,CHART,NOTES
VX For,2455090.09733,12.936,0.011,V,NO,ABS,ENSEMBLE,na,137,13.660,1.55703,na,090915,na
VX For,2455090.09994,12.959,0.010,V,NO,ABS,ENSEMBLE,na,137,13.665,1.53358,na,090915,na
VX For,2455090.10256,12.991,0.011,V,NO,ABS,ENSEMBLE,na,137,13.662,1.51102,na,090915,na
Looks like Rod has bagged a beauty!!!!
Peter
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