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Lozinskaya, N. A.; Tsybezova, V. V.; Проскурнина, М. В.; Зефиров, Н. С.

doi:10.1023/a:1023915024572

Cited by 18 publications

(4 citation statements)

References 7 publications

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“…19 Hydrobenzamide, its methoxy- and fluorine-substituted analogs were derived from the reactions of the corresponding aromatic aldehyde with ammonia. 20 Their cyano counterpart was obtained using a slightly modified procedure published elsewhere. 21 Picolinyl chloride was generated in situ by the reaction of picolinic acid with SOCl 2 in the presence of Et 3 N. 22 All other chemicals and solvents were used as purchased.…”

Section: Methodsmentioning

confidence: 99%

(Aminoalkyl)diphenylphosphine sulfides: synthesis and application as building blocks in the design of multidentate ligands for cytotoxic Pd(ii) complexes

Konovalov,

Churusova,

Aleksanyan

et al. 2023

Org. Biomol. Chem.

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Section: Methodsmentioning

confidence: 99%

(Aminoalkyl)diphenylphosphine sulfides: synthesis and application as building blocks in the design of multidentate ligands for cytotoxic Pd(ii) complexes

Konovalov,

Churusova,

Aleksanyan

et al. 2023

Org. Biomol. Chem.

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“…VdB 130 is located in projection near the northwestern border of an extended optical, radio and IR shell around Cyg OB1 (Fig. 1) (Lozinskaya & Sitnik 1988;Lozinskaya & Repin 1990;Saken et al 1992). This supershell is also clearly discernible at all wavebands observed with the Spitzer space telescope (Hora et al 2009) and at large-scale CO distribution ).…”

Section: Molecular Cloud and Ionized Hydrogen In The Vicinity Of The mentioning

confidence: 99%

Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association – I. The star cluster vdB 130 and its ambient gas and dust medium

Sitnik

Egorov

Lozinskaya

et al. 2015

Mon. Not. R. Astron. Soc.

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Stellar population and the interstellar gas-dust medium in the vicinity of the open star cluster vdB 130 are analysed using optical observations taken with the 6-m telescope of the SAO RAS and the 125-cm telescope of the SAI MSU along with the data of Spitzer and Herschel. Based on proper motions and BV and JHKs 2MASS photometric data, we select additional 36 stars as probable cluster members. Some stars in vdB 130 are classified as B stars. Our estimates of minimum colour excess, apparent distance modulus and the distance are consistent with young age (from 5 to 10 Myrs) of the cluster vdB 130. We suppose the large deviations from the conventional extinction law in the cluster direction, with R V ∼ 4 − 5. The cluster vdB 130 appears to be physically related to the supershell around Cyg OB1, a cometary CO cloud, ionized gas, and regions of infrared emission. There are a few regions of bright midinfrared emission in the vicinity of vdB 130. The largest of them is also visible on Hα and [Sii] emission maps. We suggest that the infrared blobs that coincide in projection with the head of the molecular cloud are Hii regions, excited by the cluster B-stars. Some signatures of a shock front are identified between these IR-bright regions.

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“…For example, Case & Bhattacharya [1] minimised the square deviations on Σ , and obtained a Σ −D relation with n = 2.64 ± 0.26 (for 37 'shell' remnants, including Cas A), which they commented was a considerably flatter Σ −D slope than had been obtained previously (e.g. Milne [11] derived n = 3.8, Lozinskaya [12] derived n = 3.45). However, by minimising square deviations in D, for the calibrators used by [1], n = 3.53 ± 0.33 is obtained, which is a much steeper Σ −D slope, and is consistent with previously derived slopes.…”

Section: The 'σ −D' Relationmentioning

confidence: 99%

The distribution of SNRs with galactocentric radius

Green¹

2012

AIP Conference Proceedings

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Abstract. In order to determine the Galactic distribution of supernova remnants (SNRs) there are two main difficulties: (i) there are selection effects which mean that catalogues of SNRs are not complete, and (ii) distances are not available for most SNRs, so distance estimates from the 'Σ −D' relation are used. Here I compare the observed distribution of 69 'bright' SNRs with Galactic longitude with that expected from the projection of various model Galactocentric radius distributions. This does not require distances from the 'Σ −D' relation, and selecting only 'bright' remnants aims to avoid major issues with the selection effects. Although this method does not provide a direct inversion to the 3-D distribution of SNRs in the Galaxy, it does provide useful constraints on the Galactocentric radius distribution. For a combined power-law/exponential model for SNR surface density variation with Galactocentric radius, the best fitted distributions are more concentrated towards lower radii than the distribution derived by Case & Bhattacharya [1].

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Untitled

Cited by 18 publications

References 7 publications

(Aminoalkyl)diphenylphosphine sulfides: synthesis and application as building blocks in the design of multidentate ligands for cytotoxic Pd(ii) complexes

(Aminoalkyl)diphenylphosphine sulfides: synthesis and application as building blocks in the design of multidentate ligands for cytotoxic Pd(ii) complexes

Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association – I. The star cluster vdB 130 and its ambient gas and dust medium

The distribution of SNRs with galactocentric radius

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