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Logging in every time is getting tedious and the login always taking you back to the home page instead of staying on the page you were on adds to the frustration. Definitely need a keep logged in cookie
On mobiles the login option is right at the bottom of a long list, neededing to scroll down several pages. Suggest bringing it to a prominent position at the top
Another post has disappeared 🙁
EDIT It may be related to adding complete web addresses. The post stayed when I shortened the addresses as below
Trying again
Some content which was free access previously is now members only. Is that a policy decision ?
eg
….videos/pushing-the-limits-using-commercial-spectrographs-2
….videos/using-low-resolution-spectroscopy-to-confirm-supernova-discoveries-2which I have linked to on other forums
Cheers
RobinJust added a post here, then edited it but it has disappeared ???
Robin
EDIT It was about multiple wrongly directed links on
https://britastro.org/section_information_/equipment-and-techniques-section-overview/spectroscopy
EDIT no idea where that graphic is from I just entered the full address of the page with the wrong links….section_information_/equipment-and-techniques-section-overview/spectroscopy
Multiple wrongly directed links from
https://britastro.org/section_information_/equipment-and-techniques-section-overview/spectroscopySpectroscopy workshop at the Norman Lockyer Observatory October 2015
Alpy 600 Spectrograph workshop, Kintbury, October 2016
Observers’ Workshop on Variable Stars, Photometry and Spectroscopy, 29 Sep 2018
Using low resolution spectroscopy to confirm and classify supernovae (video from BAA meeting January 2018)
Starting in Spectroscopy (video from BAA/AAVSO joint meeting on variable stars, July 2018)
Pushing the limits using commercial spectrographs (video from BAA/AAVSO joint meeting on variable stars, July 2018)
Towards full automation of high resolution spectroscopy (video from BAA/AAVSO joint meeting on variable stars, July 2018)
HST CALSPEC calibrated absolute flux spectra for converting relative intensity to FLAM unitsEDIT No idea where the graphic came from, I just entered the address of the page
“https://britastro.org/section_information_/equipment-and-techniques-section-overview/spectroscopy”Even allowing for the trailing, that looks quite a bit fainter than the mag 13 Nick reported on 5th. The adjacent bright star is SDSS J081542.48+144838.9 at g mag 15
A low resolution spectrum taken last night (3 hours exposure) showing a very broad H alpha emission with velocities up to +-12000km/s
https://britastro.org/observations/observation.php?id=20220207_205606_9d5b2259183a3d41
Cheers
Robin
Thanks Nick,
I’ve found the original preprints of Comets II are available to download from the Lunar & Planetary Institute. Plenty of reading there !
Hi Maxim,
Thanks for the reference. ( I am on a steep learning curve here !) I can understand how the Swings effect could enhance or suppress the strength of the resonance emission due to the velocity relative to the sun (The distributions are normalised relative to the intensity at the coma centre so don’t show the absolute strengths) but I don’t follow how that could alter the shape of the CN distribution. Would this be due to the resulting radiation pressure sweeping the CN away from the coma into the tail, like Sodium in 2020 F3 ?
That reference to parent molecules and the Haser model on your Fernandez page 68 did remind me of some comments from Jeff Morgenthaler of the IoIO team on my F3 cross sections.
“CN is produced from a parent molecule, likely HCN. The combination of that double process ends up extending the lifetime of CN to photodissociation (destruction by sunlight). I have not done the conversion of angular scale to distance from the comet on your night of observation, but the characteristic scale length of CN emission when comets are at 1 AU from the sun tends to be about 20,000 km. C2 is a little weirder in terms of parent molecules. It seems to have two dominant ones, leading to a flat profile in the inner few thousand km of the coma. Then it drops off with a profile slightly shorter than CN.”
So perhaps I need to consider the effect of sunlight on both the rate of production and destruction of CN and C2 and follow up on the Haser model.
Thanks
Robin
“Is CN also broken down by sunlight, though at perhaps a slower rate than C2 ?”
Actually, answering my own question it looks like that cannot be the explanation as CN is seen widely distributed in the cross section through the tail of 2020 F3. Any ideas of what is going on?
So.. I went looking for what Lee Feinberg actually said in the teleconference. He did indeed say it could be seen with binoculars in Ursa Major, but…… he was talking about the target they were going to use to collimate the mirror (HD84406)
https://www.youtube.com/watch?v=VmD8pefGG2k&t=949s 39 minutes in
To be fair, NASA do have access to some pretty large binoculars !
Phew! Now lets hope all the 126 actuators which align the mirror segments work ok. The number of moving parts in the instruments is mind boggling too. NIRSpec apparently has a matrix of a quarter of a million focal plane “microshutters”
Perhaps past citations where available could also be added as links from the list of recipients? As well as of individual interest it would reflect the overall achievements of the Association and its members as a whole.
I don’t think they are published consistently. I remember looking for my 2019 Merlin Medal in the Journal and could not find one. I recall it was not mentioned at the meeting when I received it either so AFAIK there is no public record of why I received it.!
I took another quick look, dodging the showers under poor conditions, this time with the very low resolution faint object setup.
The emission lines are very narrow (which confirms it is not a classical nova) so do not show well at the lower resolution but the blue continuum is unchanged.
The angular size of the lensed star could be inferred from the Gaia parallax, the apparent magnitude and the spectral classification.
