Search Results for 'espin telescope'

[Wayne Hawley]

A plea for assistance.
As part of the Asteroids and Remote Planet section we are trying to find the rotation period for several asteroids, most of which rotate relatively quickly however this asteroid which is around mag 15 rotates slowly. Until we get a complete lightcurve there is a lot of uncertainty, we currently have two front runners of a little over 400 hours and around 930 hours. During the next 180 hours if its the longer of the two periods we have a gap in the coverage. If you are able to obtain some images of this ateroid with or without a filter and send me the reduced images it will help us to complete the lightcurve. We have observers in the UK, Greece, Luxembourg, USA mainland, NZ and Hawaii.We are also obtaining images from the LCO network and some observers are using remote telescopes. An explanation of what we are doing is in the AARPS page on the BAA website. Images should be about 60 seconds and a minimum telescope size of 10 inch 0.25m to give a good SNR.
Thanks in advance Wayne Hawley Z09

Attachments:

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   1429-Pemba-possible-light-curve-with-much-longer-period.png
   

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   1429-Pemba-possible-light-curve-with-shorter-period.png
   

[Mr Ian David Sharp]

Hi all,

It looks like the occultation track of Leone tonight passes over my telescope at PixelSkies in Spain.

Having a C11 with an SX694 TRIUS CCD, I can’t take short, rapid exposures a la a CMOS camera, so my plan is to let it drift across the FOV. I will experiment first with am R filter but I suspect it will easily saturate. Then I will try an SII. All slightly off focus I think.

Any other tips?

Cheers
Ian.

[Alex Pratt]

‌
On https://www.virtualtelescope.eu/webtv/

Gianluca Masi, Italian astronomer and developer of “THE VIRTUAL TELESCOPE PROJECT”,
has posted the following announcement :

Next event: “Betelgeuse occultation by Leona: live view” –
12 Dec. 2023, starting at 01:00 UTC

[Jeremy Shears]

Another year on: now 4 years from the Great Dimming!

An A&A preprint appears on ArXiv today (https://arxiv.org/abs/2312.02816) shows how different layers in the star’s photosphere appeared pourturbed during the event, returning to normal in 2022.

The Great Dimming of Betelgeuse: the photosphere as revealed by tomography during the past 15 years

Daniel Jadlovský, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Jiří Krtička, K. Andrea Dupree, Andrea Chiavassa, G. Klaus Strassmeier, Katja Poppenhäger

Betelgeuse, a red supergiant star of semi-regular variability, underwent a historical minimum of brightness in February 2020, the Great Dimming. Even though the brightness has returned to the values prior to the Great Dimming by now, it continues to exhibit highly unusual behavior. Understanding the long-term atmospheric motions of Betelgeuse and its variability could be a clue to the nature of the Great Dimming and the mass-loss process in red supergiants. Our goal is to study long-term dynamics of the photosphere. We applied the tomographic method, which allows different layers in the stellar atmosphere to be probed in order to reconstruct depth-dependent velocity fields. The method is based on the construction of spectral masks by grouping spectral lines from specific optical depths. These masks are cross-correlated with the observed spectra to recover the velocity field inside each atmospheric layer. We obtained about 2700 spectra during the past 15 years, observed with the STELLA robotic telescope in Tenerife. We analysed the variability of 5 different layers of Betelgeuses photosphere. We found phase shift between the layers, as well as between the variability of velocity and photometry. The time variations of the widths of the cross-correlation function reveal propagation of two shock waves during the Great Dimming. For about 2 years after the Dimming, the time scale of variability was different between the inner and outer photospheric layers. By 2022, all the layers seemingly started to follow a similar behavior as before the Dimming, but pulsating with higher frequency corresponding with the first overtone. Combination of the extensive high-resolution spectroscopic data set with the tomographic method revealed the variable velocity fields in the photosphere of Betelgeuse, for the first time in such detail.

[Dr Paul Leyland]

It is that time of year again. A recurrent nova in M31 is due to go off again. This one has by far the shortest recurrence period known at about 1 year. I have been looking out for it for quite a while but it has never shown up when I am in La Palma. If you subscribe to 12a_Monitoring@googlegroups.com you will have seen the material below. If not, and you can image down to mag 18 or so in a reasonable time (meaning you have a 20cm telescope or larger) please consider subscribing. My http://www.astropalma.com/Projects/VS/M31N_2008-12a.html provides more information and a link to a finder chart.

Thanks, Paul

Dear colleagues,

Another year ticked off (almost)! As always, I hope you are all keeping well at this time!

Traditionally, this is an e-mail I’ve send around the start of September – this year, I am purposely sending it later as we are working toward a smaller potential eruption window. I know many of you have already been observing 12a regularly – so thanks for that!

This email is to let you all know that, yet again, we have officially restarted our ground-based optical monitoring of the remarkable M31 recurrent nova M31N 2008-12a with the aim to detect the 2023 eruption. As always, I want to extend our thanks to those of you who have already been observing over the last weeks and I want to encourage everyone to join the monitoring effort once again.

We have again secured several very early time spectroscopic observations of the 2023 eruption that require early notification of the 2023 eruption for triggering. This again includes time on the Liverpool Telescope. Our aim with these follow-up observations remains to probe the early-time physics that drive the eruption and an attempt to definitively determine the ultimate fate of M31N 2008-12a – whether one day it will explode as a Type Ia supernova or collapse to a neutron star. Your continued involvement in this project is key to all these aims! Each year we manage to get on target faster and faster, we are hoping that the heavens (and weather) align this year to start our follow-up observations within an hour of the eruption occurring – it’s ambitious, but in theory we can do it!

Last year, although we had an early detection of the eruption of 12a (https://www.astronomerstelegram.org/?read=15786) and rapid spectroscopic follow-up (https://www.astronomerstelegram.org/?read=15788), unfortunately, the geography at the time of eruption meant that we discovered the event just too late to meet the early spectroscopic goals. The LT is setup to automatically trigger spectroscopic observations of 12a as soon as we receive a report of an eruption – stopping any on-going observations at the time, we have ‘ultimate priority’ for these observations! Indeed, we have automated the whole process should the LT be the first telescope to detect the 2023 eruption!

As in previous years, below I outline in detail the monitoring and reporting structure, as well as the notifications in case of a discovery. This strategy is the same as recent years. Please follow the precise instructions because, for instance, some of us have set up email alerts based on the email subject of the discovery notification.

In previous years, the Liverpool Telescope has been a regular source of additional eruption monitoring observations but has only been the first telescope to detect three of the fifteen consecutive eruptions (2014, 2018, and 2020). Out of interest, of those 15 eruptions 8 have been detected by members of this group (the other 7 by facilities such as PTF, LT, and LCO)!

We will still be using the mailing list 12a_Monitoring@googlegroups.com for the communication within the collaboration. The finding chart and reference stars remain the same as for the previous eruption. If you have any questions don’t hesitate to contact me at M.J.Darnley@ljmu.ac.uk and I will provide clarification. Please note that the “12a” mailing list is reserved for discussions about this nova.

I hope that all of you will join again for another exciting season of watching the most remarkable nova go into eruption. Please let me know in case you will not be able to participate in this year’s campaign.

Best regards and clear skies,

Matt for the 12a Collaboration

1) The eruption date prediction

Based on an updated analysis, we expect the 2023 eruption of 12a will take place in December 2023, with the window possibly extending into early January 2024.

2) Who is coordinating

Mike Healy (M.W.Healy@ljmu.ac.uk) and I (M.J.Darnley@ljmu.ac.uk) will be coordinating the observations, but also involved and very interested will be: Allen Shafter (awshafter@gmail.com).

3) Communication strategy

For the communication within the collaboration we will use exclusively the mailing list 12a_Monitoring@googlegroups.com. The usage of the list should be restricted to notifications of (potential) discoveries, status updates from the coordinators, requests for confirmation, and urgent queries. This will reduce the email traffic for all of us. In case of non-urgent/minor questions or updates please contact me (M.J.Darnley@ljmu.ac.uk) directly.

4) Where to report upper limits and photometry?

We encourage all of you to report your upper limits to the AAVSO database, whether you are an AAVSO member or not. We have established the AAVSO database as central data collection hub for this project. We will be checking your reported upper limits frequently. Here is information on how to submit data to the AAVSO, courtesy of (former) AAVSO director Stella Kafka:

Information on how to get an AAVSO observer code and submit your data directly to the AAVSO database: To do so, you need to create an account here: https://www.aavso.org/join-aavso(under “Click Here to Join the AAVSO”).

Once you register, please request an observer code.

Please note that you don’t need to be members to get an observer code and submit data (although it would be great if everyone becomes an AAVSO member and supports the association). Observer codes are unique and help us give credit to observers who acquire observations and diagnose problems with discrepant data when needed.

In case of further questions about the AAVSO data base please contact me (M.J.Darnley@ljmu.ac.uk) or the AAVSO directly.

5) What do we need for a discovery?

To discover the eruption and notify the collaboration, you only need a reliable detection. Ideally, the nova should be clearly detected in more than one exposure. Photometry is useful, but can be done later, because we need to react fast. We are relying on your expertise and judgement about whether a detection is real. If in doubt, follow point 7 below.

Please find attached a finding chart of the nova. The finder chart image is an exceptionally deep exposure taken by the 2m Liverpool Telescope through a Sloan r’ filter, the median seeing of the 21 images combined here was around 1 arcsecond.

6) Discovery notification

If you are successful in discovering the eruption, please notify the collaboration immediately through the mailing list: 12a_Monitoring@googlegroups.com

This should be the first thing you do. CBAT entries or ATels can wait until after this (short) email. Remember that the nova is evolving fast and that we need to be very quick (particularly in triggering the follow-up observations).

Here is a template for the discovery notification. Please attach a discovery image for your stacked data and for at least 2 individual exposures. Ideally, we need a .fits file but if it speeds up the notification then a .jpg screenshot is fine.

If you can immediately provide photometry, then please do so. Otherwise send this email without photometry but start working on the photometry after sending. We will get back to you very quickly.

——————————————–

subject:

——–

M31N 2008-12a – 2023 eruption discovered!

text:

——–

Dear colleagues,

The 2023 eruption has been discovered. Please try to increase your observing cadence to monitor the light curve.

The nova was discovered on <date and time> with a magnitude of <mag> at the <observatory>. Discovery images are attached.

——————————————-

7) If you are not sure

If you are not sure whether you have discovered the nova, please contact the mailing list (12a_Monitoring@googlegroups.com) to request a confirmation. Attach your discovery image(s) and include (preliminary) photometry as well as the location of your observatory.

This scenario is meant for low signal/noise detections at the nova position. If in doubt, please send this email. We’d rather have a few false positives then missing the early stages of an eruption.
——————————————-

subject:

———

M31N 2008-12a – possible 2023 detection; requesting confirmation

text:

———

Dear colleagues,

I found a possible detection of the nova on <date and time> with a magnitude of about <mag> at the <observatory>. Discovery images are attached. Please try to confirm this detection.

——————————————-

8) Announcement and publication

The aim is to announce the discovery in an ATel as soon as possible. All photometry will also be included in a comprehensive publication in a refereed journal.

If you discover the eruption, and after notifying the collaboration, you can publish the ATel yourself or send your discovery information to the following people, one of which will publish the ATel as quickly as possible:

M.J.Darnley@ljmu.ac.uk

M.W.Healy@ljmu.ac.uk

awshafter@gmail.com

If you choose to send the ATel yourself, below is a template that you can use (including some html code in the first paragraph that you can just copy and paste). See also the ATel on the 2017—2021 eruptions:

http://www.astronomerstelegram.org/?read=11116

http://www.astronomerstelegram.org/?read=12177

http://www.astronomerstelegram.org/?read=13269

http://www.astronomerstelegram.org/?read=14130

https://www.astronomerstelegram.org/?read=15034

[Nick James]

The inner bright coma is showing quite a bit more detail now. The attached is 4 arcmin square, N up, E left, taken using the Alnitak telescope in Spain at 1906 UTC on Nov 17. There appear to be two blobs of material north of the coma. Does anyone else have any images that can confirm this?

Attachments:

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   12p_20231117_190638_ndj.jpg
   

[Nick James]

It’s cloudy here tonight but I’m getting some images from the Alnitak telescope in Spain. This outburst is different to the others and David is right that this does look like a mini 17P/Holmes. I’m assuming the faint larger disk is the gas coma which expands quickly and the bright inner disk is the slower moving dust but don’t quote me on that.

It would be an interesting object to try spectroscopy on while it is currently bright…

[Nick James]

I’ve just imaged the comet again and it was mag 9.4 on Nov 15.72 in a 34 arcsec aperture. This is a really big outburst and the comet should be a fairly easy visual target in a moderate telescope at the moment.

[Nick James]

It looks as if comet 12P/Pons-Brooks is in outburst again. I imaged it early last night from Chelmsford (Nov 14.75) and the magnitude rose from 13.6 to 12.5 in 25 minutes. My last image, on Nov 13.80 using the Alnitak Observatory telescope in Spain, shows it as 14.7.

If you have any images of 12P taken on Nov 14/15 could you please let me know so that we can build a comprehensive light curve of this event.

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   12p_20231114.png
   

[Mr Ian David Sharp]

Kevin West wrote:

SIMPLE = T / file does conform to FITS standard
Which I know is a bit of a deal breaker as they have to conform. So that’s where I am. Any thoughts please?

Hi Kevin,

I don’t understand the problem. It all looks OK to me. Here, for comparison, is one of my FITs headers after it’s been calibrated. (Captured in SG Pro, calibrated by AA8).

Cheers
Ian.

SIMPLE = T / file does conform to FITS standard
BITPIX = 16
NAXIS = 2
NAXIS1 = 2750
NAXIS2 = 2200
BZERO = 32768.0
BSCALE = 1.0
CRPIX1 = 1375.999999978
CRPIX2 = 1100.999999981
CTYPE1 = ‘RA—TAN’
CTYPE2 = ‘DEC–TAN’
OBJECT = ‘CF PEG ‘ / Object name
DATE-LOC= ‘2023-10-08T21:50:30.3930000’ / Local observation date
DATE-OBS= ‘2023-10-08T19:50:30.3930000’ / UTC observation date
IMAGETYP= ‘LIGHT ‘ / Type of frame
CREATOR = ‘Sequence Generator Pro v4.2.0.1158’ / Capture software
INSTRUME= ‘Starlight Xpress H694’ / Instrument name
ROWORDER= ‘BOTTOM-UP’
OBSERVER= ‘Ian Sharp’ / Observer name
SITENAME= ‘PixelSkies’ / Observatory name
SITEELEV= 850 / Elevation of the imaging site in meters
SITELAT = ’37 44 23.000′ / Latitude of the imaging site in degrees
SITELONG= ‘-0 38 38.000’ / Longitude of the imaging site in degrees
FOCUSER = ‘PegasusAstro ProdigyMF’ / Focuser name
FOCPOS = 5489 / Absolute focuser position
FOCTEMP = 19.48 / Focuser temperature
FWHEEL = ‘Starlight Xpress Filter Wheels’ / Filter Wheel name
FILTER = ‘L ‘ / Filter name
EXPOSURE= 60 / Exposure time in seconds
CCD-TEMP= -10.2 / Camera cooler temperature
SET-TEMP= -10 / Camera cooler target temperature
XBINNING= 1 / Camera X Bin
CCDXBIN = 1 / Camera X Bin
YBINNING= 1 / Camera Y Bin
CCDYBIN = 1 / Camera Y Bin
XPIXSZ = 4.5390625 / Pixel Width in microns (with binning)
YPIXSZ = 4.5390625 / Pixel Height in microns (with binning)
STRSZ1x1= 6 / SGPro minimum star size filter
READOUTM= ‘Standard Readout Mode’ / Camera readout mode
TELESCOP= ’10Micron Mount’ / Telescope name
RA = 325.297497442515 / Object Right Ascension in degrees
DEC = 26.2268339926879 / Object Declination in degrees
CRVAL1 = 325.2979715357
CRVAL2 = 26.20068031717
OBJCTRA = ’21 41 11.399′ / Object Right Ascension in hms
OBJCTDEC= ‘+26 13 36.602’ / Object Declination in degrees
PIERSIDE= ‘West ‘ / Side of Pier the objective is on
AIRMASS = 1.04170531837155 / Average airmass
OBJCTALT= 73.8212777777778 / Altitude of the object
CENTALT = 73.8212777777778 / Altitude of the object
FOCALLEN= 1956 / The focal length of the telescope in mm
FLIPPED = F / Is image flipped
ANGLE = 267.83 / Image angle
SCALE = 0.472905 / Image scale (arcsec / pixel)
PIXSCALE= 0.472905 / Image scale (arcsec / pixel)
AOCDEW = 10.3 / Dew Point in degrees C
AOCHUM = 75 / Humidity in %
AOCRAIN = 0 / Rain Rate in mm/hr
AOCSKYT = -28.5 / Sky Temperature in degrees C
AOCAMBT = 18.7 / Ambient Temperature in degrees C
AOCWIND = 12.5833333333333 / Wind Speed in m/s
EGAIN = 0.3 / Electrons Per ADU
STAR = ‘CF PEG’
PROCESS = ‘DK+FLAT’
CALSTAT = ‘BDF’
EQUINOX = 2000.0
CD1_1 = 4.981204779451E-006
CD1_2 = -0.0001310849482926
CD2_1 = -0.0001310385252376
CD2_2 = -4.948753747364E-006
CDELT1 = -0.0001311331670384
CDELT2 = 0.0001311783283646
CROTA1 = 0.0
CROTA2 = -87.83051432587
AVISUMIN= -33.0
AVISUMAX= 467.0
AVISUTYP= 0.0
END

[Gary Poyner]

In VS observing (and Comets too), it’s normal to give the decimal of the day following the days date. So Jul 20.82 is July 20, 19h 45m UT.

The time is written down in hours and minutes at the telescope, then the spreadsheet works out the decimal of the day when the observations are typed up. To obtain the decimal of the day, my spreadsheet multiplies the hour by 60, adds the minutes, then divides by 1440. This has been normal practice in VS observing for many years – particularly CV’s (although some observers still do report in hours and minutes).

I tend to report everything in decimal of the day these days.

Gary

[Howard Lawrence]

This is an interesting article from Sky and Telescope on satellite status and the comments are worth reading. https://skyandtelescope.org/astronomy-news/a-new-hope-taming-the-satellite-swarm-in-our-skies/

[Tim Haymes]

When observing/recording, the event will occur near 2309 UT. so best to record video from 2308 to 2310 UT in the UK (see the graphic).
For most observers with access to NTP, it would be best to use the Meinberg software to keep the computer clock sync’ed to UT.
https://www.meinbergglobal.com/english/sw/

The recording software of my choice is SharpCap, where SER or FITS images can be selected with recording between 10 and 3 fps. (dependent on the instrument and camera). With a 20cm and mono CMOS, an exposure of 100ms may be possible. All depends on transparency and light pollution levels, so the only way to tell is at the telescope. As long as the 12.6 mag target is detected clearly, a result is possible. The ARPS section can perform the analysis and help prepare a report.

Cheers – Tim
ARPS (Occultations)

[Gary Poyner]

Hi David,

Yes, it’s nice to see this star active again. I’ve had it rsing from 12.7mv on Sep 15 to 11.8mv by Oct 8, with 0.5 mags of that in the last five days.

The VSS doesn’t have a chart for V426 Sge (also known as VEND47), but you can download one from the AAVSO web site and configure it to your type of telescope.

Gary

[Dr Paul Leyland]

I am also on the astrometry.net mailing list and have been following your communications there with interest.

At present I’ve no real use for precision astrometry, using the plate solver only to find stars to within a few arcseconds which is plenty good enough for pointing a telescope and to enable APT to find a VS and its comparison sequence, then to do precision photometry.

On the odd occasion I do need good astrometry I use either Astrometrica, if it can be persuaded to work at all, or the IRAF tools.

[Dawson]

I’ve been to see Alan Heath today and helped him set up his telescope out the front of the house so he could count sunspots for Lyn. He hates to have an incomplete record.

He dropped his 1″ eyepiece and is using a 10mm one and would ideally like to see the whole disc of the Sun again, so I said I’d try and find him a 1″ (25mm) RAS thread eyepiece. He uses a Herschel wedge and also a dimming filter which screws on the top of the eyepiece, so it needs to be threaded on both ends.

If anyone has one to sell, please let me know.

Regards

James Dawson
Nottingham

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   WhatsApp-Image-2023-09-05-at-15.03.47c.jpg
   

[Jeremy Shears]

A post not about the next eruption, but about two previous ones in 1787 and 1217!

A JHA pre-print by Prof Brad Schaefer The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD appears on ArXiv today: https://arxiv.org/abs/2308.13668

He comments “T CrB has four observed eruptions in the years 1217.8, 1787.9, 1866.4, and
1946.1, plus one more expected upcoming in 2024.4±0.3. The recurrence
timescales are 7×81.4, 78.5, 79.7, and likely 78.3±0.3 years. With 9 eruptions
from 1217.8 to 1946.1, the average recurrence timescale is 80.9 years. I expect
additional eruptions within a year or two of 1706, 1625, 1544, 1462, 1381, 1299,
1137, 1055, 974, 892, 811, 730, 648, 567, 485, 404, 323, 241, 160, and 78 AD. ”

Abstract:
The famous recurrent nova (RN) T Coronae Borealis (T CrB) has had observed eruptions peaking at a visual magnitude of 2.0 in the years 1866 and 1946, while a third eruption is now expected for the year 2024.4+-0.3. Each RN has very similar light curves of eruptions that come with a fairly even-spacing in time, for which T CrB has a recurrence timescale near 80 years. So it is reasonable to look backwards in time for prior eruptions, around 1786, and so on back. I have investigated two long-lost suggestions that T CrB was seen in eruption in the years 1217 and 1787. (1) In a catalog published in 1789, the Reverend Francis Wollaston reports an astrometric position for a star that is exactly on top of T CrB. From his letters, these observations were made on at least four occassions with both a large and small telescope, within a few days before 1787 December 28. Wollaston’s limiting magnitude for his astrometry is near 7.8 mag, so T CrB would have to have been in eruption. With other transients strongly rejected, the only way that Wollaston could get the coordinates was to have measured the coordinates of T CrB itself during an eruption. (2) The 1217 event has an eyewitness report written by Abbott Burchard of Upsberg as a fast-rising stellar point-source (“stella”) in Corona Borealis that “shone with great light”, lasted for “many days”, and was ascribed as being a “wonderful sign”. This event cannot be a report of a comet, because Burchard used the term for a star (“stella”) and not for a comet, and because Burchard had the omen being very positive, with such being impossible for comets that are universally the worst of omens. The reported event is just as expected for a prior eruption of T CrB, and all other possibilities are strongly rejected, so the case for the 1217 eruption of T CrB is strong.

• This reply was modified 3 years, 1 month ago by Jeremy Shears.
• This reply was modified 3 years, 1 month ago by Jeremy Shears.

[Gerard Fox]

I have found the Geoptik Large High Quality Telescope Cover quite useful for my EQ6 & CEM70 mounts.

• This reply was modified 3 years, 2 months ago by Gerard Fox.

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[Grant Privett]

I don’t see why not – but am happy to be corrected if I am wrong.

I use a coma corrector on my telescope and do photometry.

Just be sure to always do dark subtraction and flat fielding.

[David Strange]

Forwarded:
Primarily for observers in South West UK:

Subject: [Norman Lockyer Observatory] Contact Us

You got a new response!
Name:
Damya Souami
Email:
damya.souami@obspm.fr
Comment:
Hello,
My name is Damya Souami. I am a researcher at the Observatory of Paris,. I am reaching out about a challenging (twilight and relatively high airmass) occultation event observable from your observatory.

The event is a stellar occultation by an outer solar system object that belongs to the dynamical class called the Damocloids. It is a highly eccentric (0.954) and retrograde orbit ( inclination ~125°).

On August 18th UT around 22:20 UT, 2013LU28 will be occulting a 13.1 mag star. Here is the detailed prediction https://lesia.obspm.fr/lucky-star/occ.php?p=124677 . On this page you will find the star’s coordinates as well as an interactive sky map (using Aladin).

This event is very important because of the nature of the object. The event will last at most 5.7s.
The challenging part is the fact that this event will be happening during twilight, at the the star is relatively low. The conditions (in terms of elevation) are more favourable in the UK and Ireland.
At your location, the conditions are the following elevation h10.5, azimuth A344.8, hour angle H:10h29m.

I hope there are no trees or building … or other constraints preventing you for pointing the telescope.
If you do have a fast camera, make some tests the nights before and try too et an SNR of (ideally) 5 to 10 on the star.
Observations at your location must be done between 22:10 to 22:25.

If this event is technically observable from any of your telescopes, I’ll be happy to exchange on the instrumental setup.
In case you are going through with the observation, please do not hesitate to involve students or amateurs.

All observers who participate to our campaigns are considered as collaborators, and are co-authors to our science papers.
Cheers,
Damya

—
This campaign is carried out under the “Lucky Star” umbrella. Lucky Star is an EU-funded research activity that agglomerates the efforts of the Paris, Granada and Rio teams. You might be contacted by different people from these three groups, but we are all working together. See Lucky Star web page for details:
http://lesia.obspm.fr/lucky-star/

——————————————————————————————————————
Dr. Damya Souami — Ph.D in Celestial Mechanics
Fulbright Visiting Scholar (2022 – 2023) at UC Berkeley
CNRS Researcher (Chargée de Recherche) at LESIA/ Observatoire de Paris

Member of the ACROSS (collaborative occultation observations for NEAs) ESA funded project – https://lagrange.oca.eu/fr/home-across

Member of the ERC Lucky Star project http://lesia.obspm.fr/lucky-star/

Affiliated with: NAXYS – Namur Center for Complex Systems-, UNamur, Belgium.
ca.linkedin.com/in/damyasouami/