jahr_2026 – Deep Sky Elements of Creation

Astronomical images of the year 2026

The supernova remnant Sh2-224, also known as SNR G166.0+04.3 or LBN 769 (Crop), is located in the constellation Auriga.

The supernova remnant Sh2-224 aka SNR G166.0+04.3 aka LBN 769 (Crop) It lies in the constellation Auriga, and is also called the "Chinese Hat".
The distance to the SNR is approximately 14,700 light-years.
The SNR spans approximately 235 light-years.
The supernova remnant is extremely faint with an apparent brightness of 17.65 mag and is therefore very challenging for amateur astrophotographers.

RA: 05 26 48.2
DEC: +42 52 59.4

Taken by me on December 14, 2025 at the Steyersberger Schwaig near the Kranichberger Hütte at an altitude of 1536m and on January 18, 2026 on the Ebenwaldhöhe (1030m) in Lower Austria.
Total exposure time: 12 hours 59 minutes.
Exposure and filters: Red 20x60sec., Green 20x60sec., Blue 19x60sec., Ha 11x1200sec., OIII 12x1200sec., SII 13x1200sec..
Takahashi Epsilon 160ED, QHY268M, QHYCFW3, Ioptron iEQ45, MGEN2, MFOC2, Baader LRGB, Ha, OIII, SII CMOS-optimized Filter 6,5nm f/2.
Development in SHO with RGB stars.
Tools used: PI (Mars) & PS & N.I.N.A..
Revised version in SHO on January 29, 2026.

The Rosette Nebula NGC 2244 is a diffuse emission nebula in the constellation Monoceros.

NGC 2244 in SHO with lume and RGB stars.

NGC 2244 in LRGB without Ha.

The Rosette Nebula NGC 2244 is a diffuse emission nebula in the constellation Monoceros.
At the center of the nebula is the open star cluster NGC 2244.
The young star cluster illuminates the entire surrounding area, approximately 100 light-years in diameter, from the center of the Rosette Nebula.
The star cluster and nebula are 5200 light-years away from us. The nebula is therefore significantly brighter and larger than the Great Orion Nebula.
The Chandra X-ray Observatory has discovered more than 2500 protostars in the nebula.
The two brightest stars in the star cluster NGC 2244 have 400,000 to 450,000 times the luminosity of the sun.
The young O and B stars are pushing the bubble, which is currently about 40 light-years in size, apart at 50 to 100 km/h.

RA: 06 31 53.6
DEC: +04 56 32.9

Photographed by me in 2021 at Brunnalm, in 2022 at Brunnalm and Geschriebenstein, and on January 22, 2026 at Steyersberger Schwaig (1400m) in Lower Austria.
Exposure and filters: Lum 16x180ec., Lum 38x120sec., Lum 50x60sec., Red 34x120sec., Red 16x60sec., Green 31x120sec., Green 16x60sec.,
Blue 30x120sec., Blue 17x60sec., Ha 12x360sec., Ha 13x300sec., OIII 7x360sec., OIII 17x300sec., SII 15x300sec..
Total exposure time SHO: 12h 32min..
Total exposure time LRGB without Ha: 6h 53min..
Takahashi Epsilon 160ED, QHY268M, QHYCFW3, Ioptron iEQ45, Lacerta MGEN2, Lacerta MFOC2, Baader LRGB, Ha, OIII, SII CMOS-optimized Filter 6,5nm f/2.
Elaboration in SHO with RGB stars and lumens, and in LRGB without Ha.
Tools used: PI (Mars) & PS & N.I.N.A..
Prepared on January 25, 2026.

(c) Herfried Exl
https://www.exl.at/

WR 134 is a variable Wolf-Rayet star in Cygnus.

WR 134 in SHO with RGB stars.

WR 134 negativ annotated.

WR 134 also known as HD 191765 or as variable star V1769 Cygni, is an extremely massive, hot, and unstable giant star in the constellation Cygnus. It is located approximately 6,200 light-years away from us. WR 134 is a variable Wolf-Rayet star.
It belongs to the extremely hot and massive stars that are in a late stage of their stellar evolution. It shines about 400,000 times brighter than our Sun. Its surface temperature is over 63,000 Kelvin. It has five times the radius of the Sun.
Driven by extreme radiation and fast stellar winds of 2,600 km/sec (over 9 million km/h), it continuously ejects its outer hydrogen shells. WR 134 has almost completely expelled its hydrogen supply into space or fused it in its core. It is now burning heavier elements like helium. In the astronomically near future (within the next hundred thousand years), the core will collapse. The star will explode as a Type Ib or Ic supernova. In these types, hydrogen is completely absent from the explosion spectrum. After the explosion, only a black hole or a neutron star will remain of the original giant star.

RA: 20 10 15.1
DEC: +36 10 50.6

Recorded by me on July 11th, 12th and 13th, 2026 at the Fuscher Törl. at an altitude of approximately 2400m, in the beautiful Austrian Alps.
Exposure and filters: Red 20x60sec., Green 24x60sec., Blue 19x60sec., Lum: 65x30sec., Ha 25x600sec., OIII 21x600sec., SII 18x600sec..
SHO Total exposure time: 12 hours 17 minutes.
Takahashi Epsilon 160ED, QHY268M, QHYCFW3, Ioptron iEQ45, MGEN2, MFOC2, Baader LRGB, Ha, OIII, SII CMOS-optimized Filter 6,5nm f/2.
Development in SHO with RGB stars.
Tools used: PI (Mars) & PS & N.I.N.A..
Prepared on July 18, 2026.

IC 1318, also known as the Gamma Cygni Nebula or Butterfly Nebula, is shown here in SHO.

IC 1318 in SHO with RGB stars.

IC 1318 negativ annotated.

IC 1318, also known as the Gamma Cygni Nebula or Butterfly Nebula, is shown here in SHO.
This emission nebula is located in the constellation Cygnus, approximately 5,000 light-years away. The pronounced H-alpha region extends over about 100 light-years. Far in front of the nebula region lies the helle Stern Sadr (Gamma Cygni), which is why the area is also called the "Sadr Region." A prominent dark cloud of cold, dense gas and interstellar dust (LDN 889) cuts through the nebula. This dark cloud divides the glow into two halves that resemble the wings of a butterfly (IC 1318B and IC 1318C). With a little imagination, the complex resembles a butterfly, hence the alternative name "Butterfly Nebula."

RA: 20 25 23.7
DEC: +40 12 57.1

Taken by me on August 12th and 13th, 2026 on the Fuscher Törl at an altitude of approximately 2400m, in the beautiful Austrian Alps.
Exposure and filters: Red 18x60sec., Green 18x60sec., Blue 18x60sec., Ha 9x900sec., OIII 9x900sec., SII 10x900sec.
Total exposure time: 7 hours 54 minutes.
Takahashi Epsilon 160ED, QHY268M, QHYCFW3, Ioptron iEQ45, MGEN2, MFOC2, Baader LRGB, Ha, OIII, SII CMOS-optimized Filter 6,5nm f/2. Elaborated in SHO with RGB stars.
Tools used: PI (Mars) & PS & N.I.N.A.
Prepared on August 18, 2026.