About Astrojohn

I am a science geek! Interests Astronomy, Skiing, Philosophy, basically any form of technology including writing automation software for my observatory. I will also share this with others using the same EQMOD/Astroart tool set.

Slideshow

Freeware!

Observation Manager Click to join AA5ObsMgr

Click to join AA5ObsMgr

My First Test spectra using SA200

A0 spectra.

SA200 spectra of an A0 star Phad. Marked line is Hydrogen beta.

Exposure is 1.5 seconds Using the RC astrograph and Trius H694 with SA200 in the filter wheel.

 

19th March M51

M51

M51 2X300sec per colour

Just a quick image as I was trying to set up my new SA200.
Without much success!!

Just about to start a new project and my camera has a problem!

Cosmic ray strike on my camera chip!!:

Ok just had a message from Starlight Xpress about this:
It is an increase in dark current caused by a high energy particle striking the chip and causing a small flaw in the crystal structure.
Clearly not a lot you can do about this. (maybe wrap the camera up in lead when not in use, however, if it has got through the earth a bit of lead will not be very effective) It is this sort of particle that causes damage to DNA and also expensive cameras.

Horsehead Nebular – Last night 150 sec X 3 per colour

AAVSO Award!

Time flies when you are busy!!

Minimal Observation Manager Freeware added to download.

Version 9.12c is in downloads now.   Minimal configuration with only essential files in folder.

Still needs to be configured for your system.

 

All the best

John

 

Quick Monochrome image of the Triangulum Pinwheel -PGC 5818 in V filter.

 

Very short exposure to look for Supernova on 19 Nov 2017!Nearly 3 million Light Years away (NGC 0589)

Very core of our nearest Galaxy – Andromeda at 2.5 Million Light years.

Bit too big for my field of view (26′ by 21′). But nice pic of the inner dust lanes also 19 Nov 2017!

Right overhead at this time of year, so anyone with a mount and a camera with telephoto and FOV of about 2.5degrees, now is the time to image this spectacular sight.

 

Variable Star V0470 Cam – Interesting Light Curve

Light Curve

Light Curve

588733main_binary-stars-lightcurve

This data taken 12 November 2017 -(Data points on BAA Site)

But interesting shape of curve.  You can see the secondary eclipse of the dimmer and smaller star.

 

Part of the Veil Nebula – Moon 75%!

Veil nebula is a cloud of dust and ionised gas (Sulphur Oxygen and Hydrogen) in the constellation of Cygnus.  It contains a radio source and is about 1470 light years away.

Veil

Veil Nebula

Even more accurate binary data using AA6 SP3 and new camera.

UX UMA new data using new camera and new software AA6 SP3.

UXUMA

The zero point is Mag 14 the time is 2017-08-27T 23:16:19.5′ / LT for start of image exposure 80sec.  The orange is the check star.  The measurement is done against 3 reference stars from AAVSO.

V Filter (Green) and the setup was Camera Trius H694 and 8inch RC Astrograph from Altair Astro.

This is quite a fast orbital period at 0.19 days.

UXUMA 13 36 40.9 +51 54 49.5 Max12.57 Min14.15 P= 0.19667128 Type=EA/WD+NL

Algol Type EA

Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes.

WD

Systems with white-dwarf components.

NL

Novalike variables, which are insufficiently studied objects resembling novae by the characteristics of their light changes or
by spectral features. This type includes, in addition to variables showing novalike outbursts, objects with no bursts ever
observed; the spectra of novalike variables resemble those of old novae, and small light changes resemble those typical for old
novae at minimum light. However, quite often a detailed investigation makes it possible to reclassify some representatives
of this highly inhomogeneous group of objects into other types.