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2019 yılında başlayan ve ardından dünya çapında bir salgın olan COVID-19, küresel anlamda hem ekonomik hem de sosyal açıdan negatif sonuçlar oluşturmuştur. Yaşanan bu gelişmelerden hemen hemen her sektör etkilenmiş olup, Gıda, İçecek ve Tütün Sektörü de bu sektörler arasında yer almaktadır. Çalışma ile ulaşılmaya çalışılan, yaşanan gelişmelerin beraberinde Borsa İstanbul (BİST)’a bağlı Gıda, İçecek ve Tütün Sektöründe yer alan şirketlerin, COVID-19 pandemi dönemini kapsayan 2019-2021 yıllarında nasıl etkilendiklerinin ortaya konulmasıdır. Çalışmada kullanılan yedi adet finansal oran, Kamu Aydınlatma Platformu (KAP)’ndan elde edilen finansal raporlar üzerinden oluşturulmuş; elde edilen oranlar çalışmada uygulanan yöntem olan Gri İlişkisel Analiz kapsamında kullanılmıştır. Uygulama sonucunda ilgili sektördeki şirketlerin yıllar içerisindeki sıralamaları ortaya konulmuş ve değerlendirmeleri yapılmıştır. Araştırmaya göre; bazı şirketlerin bu dönemi avantaja çevirdiği, bazılarının ise değişime karşı yanıt veremediği sonucuna varılmıştır. Pandeminin etkilemediği düşünülen şirketlerin ise güçlü bir finansal yapıya sahip olduğu gözlemlenmiştir.

We present full spectral scans from 200 to 670 μm of 26 Class 0+I protostellar sources obtained with Herschel-SPIRE as part of the “COPS-SPIRE” Open Time program, complementary to the DIGIT and WISH Key Programs. Based on our nearly continuous, line-free spectra from 200 to 670 μm, the calculated bolometric luminosities (Lbol) increase by 50% on average, and the bolometric temperatures (Tbol) decrease by 10% on average, in comparison with the measurements without Herschel. Fifteen protostars have the same class using Tbol and Lbol/Lsmm. We identify rotational transitions of CO lines from to , along with emission lines of 13CO, HCO+, H2O, and [C i]. The ratios of 12CO to 13CO indicate that 12CO emission remains optically thick for Jup < 13. We fit up to four components of temperature from the rotational diagram with flexible break points to separate the components. The distribution of rotational temperatures shows a primary population around 100 K with a secondary population at ∼350 K. We quantify the correlations of each line pair found in our data set and find that the strength of the correlation of CO lines decreases as the difference between J levels between two CO lines increases. The multiple origins of CO emission previously revealed by velocity-resolved profiles are consistent with this smooth distribution if each physical component contributes to a wide range of CO lines with significant overlap in the CO ladder. We investigate the spatial extent of CO emission and find that the morphology is more centrally peaked and less bipolar at high-J lines. We find the CO emission observed with SPIRE related to outflows, which consists of two components, the entrained gas and shocked gas, as revealed by our rotational diagram analysis, as well as the studies with velocity-resolved CO emission. [ABSTRACT FROM AUTHOR]

We present the first large-scale high angular resolution survey of ionized nitrogen in the Galactic Plane through emission of its two fine structure transitions ([N ii]) at 122 and 205 μm. The observations were largely obtained with the PACS instrument onboard the Herschel Space Observatory. The lines of sight were in the Galactic plane, following those of the Herschel OTKP project GOT C+. Both lines are reliably detected at the 10−8–10−7 Wm−2 sr−1 level over the range –60° ≤ l ≤ 60°. The rms of the intensity among the 25 PACS spaxels of a given pointing is typically less than one third of the mean intensity, showing that the emission is extended. [N ii] is produced in gas in which hydrogen is ionized, and collisional excitation is by electrons. The ratio of the two fine structure transitions provides a direct measurement of the electron density, yielding n(e) largely in the range 10–50 cm−3 with an average value of 29 cm−3 and N+ column densities 1016–1017 cm−2. [N ii] emission is highly correlated with that of [C ii], and we calculate that between 1/3 and 1/2 of the [C ii] emission is associated with the ionized gas. The relatively high electron densities indicate that the source of the [N ii] emission is not the warm ionized medium (WIM), which has electron densities more than 100 times smaller. Possible origins of the observed [N ii] include the ionized surfaces of dense atomic and molecular clouds, the extended low-density envelopes of H ii regions, and low-filling factor high-density fluctuations of the WIM. [ABSTRACT FROM AUTHOR]