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I remember that too, though I think I saw it in the physics department. (I was a physics undergrad there at the time)
Hi Hugh,
Digging out the report I see Aldebaran was recorded at 45 deg altitude
I dont think scintillation effects are directional are they ? I would expect the effect to be independent of the slit orientation. Orientating the slit vertically relative to the horizon (the paralactic angle) will help with atmospheric dispersion problems though which can give systematic errors due to selective sampling by wavelength at the slit.
Cheers
Robin
EDIT: Actually thinking about it a bit more, I think there are two potential effects here.
Movement of the star image coupled with selective sampling at the slit due to atmospheric dispersion which could be reduced by orientating the slit
Distortion of the spectrum due to scintillation which is seen even in the absence of the slit (eg in Star Analyser spectra) and is seen visually as apparent colour changes in the star
The slit normally defines the location of a given wavelength in the spectrum but if the slit is wider than the star image then I guess there could be some wavelength shift between exposures due to scintillation. To avoid scintillation problems (and uneven coverage of the slit due to guiding errors) I normally accumulate at least 1 min total exposure time for a spectrum (which for bright targets at low resolution can be in shorter sub exposures), though this is not based on any scientific analysis.(I see I only used 30 sec for eps Tau in this particular exercise)
https://britastro.org/sites/default/files/attachments/ALPY600_MILES_tests_20161105.pdf
I see campaign announcements and requests for spectra coming from many directions with varying degrees of formality. (The ARAS forum for example has specific areas for campaigns and alerts). I have relayed details of some of them on this forum that I have either received direct or seen elsewhere but they can tend to get lost as they eventually scroll off the bottom of the page.
A sticky post which would stay at the top of the spectroscopy section of the forum that anyone could add to if they come across campaigns might work. (Andy and I did try this with my post on target results for ALPY observing and data reduction but it seems to have come unstuck). Adding information about a campaign announced elsewhere would not oblige the poster to coordinate it or follow it up unless they wanted to take on that responsibility. It would be up to the individual contributor to do that with the PI concerned.
Here are a few examples from me on this forum
https://britastro.org/node/16683
https://britastro.org/node/15540
https://britastro.org/node/11637
https://britastro.org/node/11372
also some run by Ernst Pollman eg
https://britastro.org/node/10809
https://britastro.org/node/10613
https://britastro.org/node/10539
Cheers
Robin
An ALPY 600 spectrum in poor conditions (thin cloud) shows a blue continuum, weak H beta and gamma in absorption and no detectable H alpha
Thanks Nick,
Just to finally put this one to bed, I checked the reflectance spectrum in a 3 arcsec window at the centre where the nucleus would be if it were detectable and compared it with the region between 5-10 arcsec from the centre where the reflectance component is still strong but outside the nucleus. They both show the same trend of decreasing reflectance towards the blue so there is no evidence of the nucleus in the spectrum. I am a bit surprised about the dust reflectance spectrum though. I had expected perhaps the opposite trend with enhanced scattering in the blue.
Cheers
Robin
I’ve found this reference for a measurement of the nucleus by the HST
http://adsabs.harvard.edu/abs/1998A&A…335L..25L
“ The color of the nucleus is moderately red with a gradient of 10% per 1000 Angstroms at optical wavelengths”
which is consistent with my measurement of the reflectance spectrum of the inner region. This is not proof that we are seeing the nucleus of course but the similarity is interesting
Robin
Hi Nick,
A figure I have seen for the diameter of the nucleus is 1.2km so a quick back of envelope calculation using the brightness of the moon as a reference and assuming the same albedo suggests that the naked nucleus would have a brightness of ~ mag 12 currently.
(distance ratio)^2 ~1000. x (diameter ratio)^2 ~10^7 = 10^10 = ~ 25 mag + mag -13 = ~ mag 12
(corrected)
which is in the ball park of what I would have guestimated it to be from the guider image. I suspect you are right though and the nucleus is indeed hidden from view by dust.
That green channel profile includes a lot of Swan band emission. Here is a vertical slice through the spectrum in a region devoid of emission lines.
It is much narrower with the reflected/scattered component mostly confined close to the centre in a region with FWHM ~ 8arcsec. There is some spread, presumably dust, but approximately 30% of the total flux comes from a region similar in width to that produced by a star in the spectrograph which with my setup is typically ~5 arcsec FWHM (wider than a normal image due to astigmatism in the spectrograph optics and guiding errors)
Cheers
Robin
I have now approximately subtracted the emission component from the spectrum of the central 6 arcsec and divided it by the solar spectrum to produce a reflectance spectrum.
It looks similar to some asteroid reflectance spectra. Since the central region is so condensed and from images there does not appear to be much dust is it possibly representative of the comet nucleus albedo or is it just scattering from dust of a particular particle size distribution? Does anyone have a feel for how bright the nucleus would appear in reflected sunlight at this distance if not active?
Robin
Here are my reduced spectra.
The diffuse coma integrated along the slit above and below the bright condensed region between 15 and 105 arcsec from the centre. Since the coma extended beyond the length of the slit the sky background was measured separately and subtracted. All the usual molecular components are there (CN is particularly intense in the UV) but no obvious Sodium.
The bright central region (6 arcsec diameter), again with the separately measured sky background subtracted showing the same emission components seen in the outer coma superimposed on a continuum spectrum with absorption lines.
The overall shape of the continuum and the absorption features match that of the solar spectrum (here compared with a solar analogue star taken the same night), though there appears to be a lack of flux from the comet around 4000-5000A ie the reflected light from the comet is deficient in the blue part of the spectrum
Robin
I cast it to my TV and wound up the volume. It was almost like sitting at the back of the theatre. Thanks to all who made this work
Here are some comparisons from the BAA database. (quick and dirty, no helio or telluric or continuum corrections)
“But on the ARAS databse…..the link for T Tauri is greyed out, and the direct link from the home page goes to a broken link..?”
Yes I noticed that. I have put a note on the thread asking it to be fixed. A timely reminder to everyone to mirror their results in a reliable long term database like the BAA one ! (mine and GJF are in there)
Cheers
Robin
Some of the emission also comes from a nebula surrounding T Tauri see my spectrum image here for example
http://www.spectro-aras.com/forum/viewtopic.php?f=5&t=1033&start=10#p4659
so perhaps what you see in these forbidden lines depends on how tightly you set the binning and sky background regions and how the slit is orientated
Robin
Hi Kevin
There is a series of around 35 spectra of the H alpha region from me and Joan Guarro Flo covering December 2014- March 2015 in the database. (I think taken as part of a Pro-Am project but I forget exactly what, I will look it up) How does yours compare ?
Robin
EDIT they were taken as part of this project (I actually made a note on the spectra in the database, seen if you tick to see all fields)
requested by Hans Moritz Guenther http://www.spectro-aras.com/forum/viewtopic.php?f=5&t=1033
A nice looking instrument Tony.
I like the idea of a high(ish) resolution version. Like the LHIRES, the chromatic aberrations should be less of an issue. The foot of the lamp lines look rather broad though. Do you think this is down to the quality of the optics? (I think I remember seeing something similar with a batch LHIRES which had poor quality doublet lenses, seen as an “elephant’s foot” shaped lines) . What focal ratio are you running ?
Did you see the results Terry Bohlsen recently posted from his version at similar resolution (presumably also with an 1800 l/mm grating) on ARAS ?
http://www.spectro-aras.com/forum/viewtopic.php?f=5&t=2172#p11890
Cheers
Robin
Here is the reduced spectrum. (red, filtered to R~300 resolution)
mag ~17 is the faintest target I have attempted with the ALPY600 setup and the SNR is very low. The broad H alpha line is obvious though and other Balmer lines are present too. I have also marked the Fe II curtain lines though they are only marginally detected above the noise.
Cheers
Robin
Here is a raw spectrum image from tonight (ALPY 600, 6600s total exposure.) It is very faint but the broad H alpha emission is clear. I will try to reduce it to see what else I can pick out
Robin
Went for a spectrum last night with the ALPY 200 but found that a series of power cuts during the storm yesterday had corrupted the observatory computer drive. 15.6 is bright for an M31 nova so definitely worth trying for even with a standard ALPY and novae spectra still show strong emission features later on even when they start to fade in measured brightness.
Robin
