Flash palsu di galaksi terjauh GN-z11 ternyata merupakan pantulan dari booster block. Tentang masalah sampah luar angkasa

Alam semesta awal mungkin adalah salah satu era kosmologis yang paling menarik, di mana kosmos yang masih ada saat ini terbentuk. Diyakini bahwa era ini berlangsung sekitar satu miliar tahun, dan selama periode ini dari Big Bang, Semesta berhasil membangun serangkaian galaksi, bertahan dari kelahiran dan kematian bintang-bintang pertama, dan juga menyaksikan kemunculan bintang-bintang besar pertama. galaksi dan lubang hitam. Kita tahu sejarah Semesta itu bukan dari buku, tetapi amati dengan mata kepala sendiri - berkat kecepatan cahaya yang terbatas, sebuah kosmos muda terletak jauh dari kita, yang cahayanya bergerak melalui zaman dan jarak.

Anda dapat menulis pertanyaan atau komentar apa pun di komentar. Saya juga terbuka untuk dialog pribadi di  telegram  atau percakapan di  obrolan kami . Saya juga memiliki  saluran telegram  tentang kosmologi.

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1. «The GN-z11 flash event can be a satellite glint»‎, Nir et al. (arXiv.org: 2102.04466);

   
   
   
   
   

2. «GN-z11-flash was a signal from a man-made satellite not a gamma-ray burst at redshift 11»‎, Michalowski et al. (arXiv.org: 2102.13164).

   
   
   
   
   

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Detection of emission lines. We first verify the detection of the UV continuum emission by stacking the 2D K-band spectrum along the wavelength direction. We detect a signal with a 5.1σ significance at the expected spatial position of the GN-z11 UV continuum (Fig. 1). We also see the standard negative-positive-negative pattern in Fig. 1b. In our ABBA observing mode, the separation between the A and B positions was 3", or ~16.7 pixels. The peak of the positive signal is roughly at x ~ 58 in Fig. 1b, so we expect to see two negative signals at x ~ 41 and 75, respectively. The negative signal at x ~ 41 is clearly seen. We can also see the negative signal at x ~ 75, although it is in a big trough that makes it less obvious. We search for emission lines in the K-band 2D spectrum and first identify a strong (5.3σ significance) line emission feature at about 22823 Å. Meanwhile, we detect a weaker (2.6σ significance), nearby line at 22797 Å. This pair of lines can be explained as the [C III] l1907, C III] l1909 doublet at z = 10.957. We would not have claimed a 2.6σ line as a detection if this line does not form a [C III], C III] doublet that is commonly seen at high redshift. We then search for >3σ lines that are associated with this redshift, and detect a line (3.3σ) at ~19922 Å that is consistent with O III] l1666 (Extended Data Fig. 3). We do not detect any other lines in the spectrum at greater than 3σ significance. If the two weak detections of 3.3σ and 2.6σ are not considered, the strongest line with the 5.3σ detection can be explained as [C III] l1907 at z = 10.970 or C III] l1909 at z = 10.957. If this line is [C III] l1907 at z = 10.970, we would expect to detect C III] l1909 with significance of ≥ 3σ, because the largest flux ratio of [C III] l1907 to C III] l1909 is about 1.6 in regular environments. Since we did not detect the expected C III] l1909 emission, the 5.3σ line is not likely [C III] l1907. Therefore, we interpret the line pair at 22797 and 22823 Å as the [C III] l1907, C III] l1909 doublet and the line at 19922 Å as O III] l1666 at z = 10.957.

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[1] Evidence for GN-z11 as a luminous galaxy at redshift 10.957 / Linhua Jiang, Nobunari Kashikawa, Shu Wang et al. // Nature Astronomy. –– 2020. –– Dec. –– Vol. 5, no. 3. ––P. 256–261. –– Access mode: http://dx.doi.org/10.1038/s41550-020-01275-y;

[2] Michalowski Micha l J., Kami ́nski Krzysztof, Kami ́nska Monika K., Wnuk Edwin. GN-z11-flash was a signal from a man-made satellite not a gamma-ray burst at redshift 11. –– 2021. ––2102.13164;

[3] Nir Guy, Ofek Eran O., Gal-Yam Avishay. Acara GN-z11-Flash Bisa Menjadi Kilatan Satelit. –– 2021. –– 2102.04466;

[4] Galaksi yang sangat terang pada z = 11.1 diukur dengan spektroskopi grismspektroskopi Teleskop Luar Angkasa Hubble / PA Oesch, G. Brammer, PG van Dokkum et al. // Jurnal Astrofisika. –– 2016. –– Mar. –– Jil. 819, tidak. 2. –– Hal. 129. –– Mode akses: http://dx.doi.org/10.3847/0004-637X/819/2/129 .