Extinctions and Distances to Dark Clouds from 2MASS, MegaCam and IPHAS Surveys: LDN 1525 in the Direction of the Aur OB1 Association

Straižys, V.; Drew, J. E.; Laugalys, V.

doi:10.1515/astro-2017-0420

Cited by 5 publications

(5 citation statements)

References 15 publications

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“…There is a gradient from A V = 1.5 − 2 mag in the north-east part of the nebula to A V > 4 mag in the south-west part. The A V value in the direction of the ionizing star is ≈ 4 mag, consistent with the value found by Straižys et al (2010). The typical uncertainty of the A V value is about 0.2 mag, which is less than 6% of the minimum A V value found in the north-west part of the nebula.…”

Section: Dust Temperature and Column Densitysupporting

confidence: 89%

“…They also reported a north-south radial velocity gradient of the ionized gas, although this was not confirmed by recent observations of RRLs by Anderson et al (2019). Straižys et al (2010) determined the interstellar extinction towards the ionizing star to be A V = 3.7 mag. Esteban & García-Rojas (2018) measured the physical parameters of the nebula with optical slit spectroscopy, and found n e =120 cm −3 from the [S ii] λλ6716, 6731 lines and T e in the range from 7100 to 11900 K, depending on the line ratio used ([N ii], [S ii], [O ii] or [O iii] lines).…”

Section: Introductionmentioning

confidence: 73%

“…The H ii region Sh2-235 (S235 hereafter, Sharpless 1959) is the brightest H ii region among four close emission nebulae (the others being Sh2-231, Sh2-232 and Sh2-233) located in the giant molecular cloud G174+2.5 (Ladeyschikov et al 2016) in the direction of the Aur OB1 association (Straižys et al 2010) in the Perseus Spiral Arm. S235 and its surroundings are a region of active star formation (see e.g.…”

Section: Introductionmentioning

confidence: 99%

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3D structure of HII region Sh2-235 from tunable-filter optical observations

Kirsanova,

Boley,

Moiseev

et al. 2019

Preprint

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We present observations of the Hα, Hβ, [S ii] λλ6716, 6731 and [N ii] λ6583 emission lines in the galactic H ii region Sh2-235 with the Mapper of Narrow Galaxy Lines (MaNGaL), a tunable filter at the 1-m telescope of Special Astrophysical Observatory of the Russian Academy of Sciences. We show that the H ii region is obscured by neutral material with A V ≈ 2 − 4 mag. The area with the highest A V is situated to the south-west from the ionizing star and coincides with a maximum detected electron density of 150 cm −3 . The combination of these results with archive AKARI farinfrared data allows us to estimate the contribution of the front and rear walls to the total column density of neutral material in S235, and explain the three-dimensional structure of the region. The H ii region consist of a denser, more compact portion deeply embedded in the neutral medium and the less dense and obscured gas. The front and rear walls of the H ii region are inhomogeneous, with the material in the rear wall having a higher column density. We find a two-sided photodissociation region in the dense clump S235 East 1, illuminated by a UV field with G 0 = 50 − 70 and 200 in the western and eastern parts, respectively.

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Section: Dust Temperature and Column Densitysupporting

confidence: 89%

Section: Introductionmentioning

confidence: 73%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

3D structure of HII region Sh2-235 from tunable-filter optical observations

Kirsanova,

Boley,

Moiseev

et al. 2019

Preprint

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“…Within uncertainties these objects may belong to the Perseus arm. Straižys, Drew & Laugalys (2010) suggest that Sh2-231 may belong to the Perseus arm, but they found a distance of 1.3 kpc for the other nebulae, which agree with the distance estimated by Humphreys (1978) for Aur OB1. This value is often assumed as the distance of objects in Aur OB1.…”

Section: Ob Associationssupporting

confidence: 75%

Towards a census of the Galactic anticentre star clusters - II. Exploring lower overdensities

Camargo

Bonatto

Bica

2012

Monthly Notices of the Royal Astronomical Society

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We investigate the nature of 48 low‐level stellar overdensities (from Froebrich, Scholz and Raftery catalogue – FSR07) projected towards the Galactic anticentre and derive fundamental parameters for the confirmed clusters, thus improving the open cluster (OC) census in that direction. Parameters are derived with field‐star decontaminated photometry, colour–magnitude filters and stellar radial density profiles. Among the 48 targets, we identified 18 star clusters, six previously studied OCs and seven probable clusters that require deeper photometry to establish the nature. We discovered seven new clusters, six of them forming an association of clusters with BPI 14, FSR 777, Kronberger 1 and Stock 8 in the region of the nebula IC 417 and related to the Aur OB2 association, and one embedded in the nebula Sh2‐229. We also derive parameters for these three non‐FSR07 clusters, because they are important in determining the structure of the Galactic anticentre. Thus, 58 objects are analysed in this work and we could derive fundamental parameters for 28 of them. The scenario in the IC 417 star‐forming region is consistent with a sequential event. FSR 888 and FSR 890 are embedded in Sh2‐249 within the Gem OB1 association. According to the distance derived for these clusters and those in the association of clusters, both Aur OB2 and Gem OB1 are located in the Perseus arm.

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“…Kang et al (2012) adopt a distance of 1.8 kpc, after Evans & Blair (1981). However, a recent comprehensive study of the extinction in this area (Straižys et al 2010) finds a lower distance of 1.3 kpc for the complex (though these authors suggest that Sh 2-231 may not belong to the complex, but rather be a background object with a much higher distance). Since this distance is compatible with the estimate for Aur OB1 found by Humphreys (1978) from a few isolated OB stars, Straižys et al (2010) identify the complex as the core of Aur OB1.…”

Section: History Of Star Formation In the Regionmentioning

confidence: 97%

Open clusters in Auriga OB2

Marco

Negueruela

2016

Mon. Not. R. Astron. Soc.

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We study the area around the H II region Sh 2-234, including the young open cluster Stock 8, to investigate the extent and definition of the association Aur OB2 and the possible role of triggering in massive cluster formation. We obtained Strömgren and J, H, K S photometry for Stock 8 and Strömgren photometry for two other cluster candidates in the area, which we confirm as young open clusters and name Alicante 11 and Alicante 12. We took spectroscopy of ∼33 early-type stars in the area, including the brightest cluster members. We calculate a common distance of 2.80 +0.27 −0.24 kpc for the three open clusters and surrounding association. We derive an age 4-6 Ma for Stock 8, and do not find a significantly different age for the other clusters or the association. The star LS V +34• 23, with spectral type O8 II(f), is likely the main source of ionization of Sh 2-234. We observe an important population of pre-mainsequence stars, some of them with discs, associated with the B-type members lying on the main sequence. We interpret the region as an area of recent star formation with some residual and very localized ongoing star formation. We do not find evidence for sequential star formation on a large scale. The classical definition of Aur OB2 has to be reconsidered, because its two main open clusters, Stock 8 and NGC 1893, are not at the same distance. Stock 8 is probably located in the Perseus arm, but other nearby H II regions whose distances also place them in this arm show quite different distances and radial velocities and, therefore, are not connected.

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Extinctions and Distances to Dark Clouds from 2MASS, MegaCam and IPHAS Surveys: LDN 1525 in the Direction of the Aur OB1 Association

Abstract: The possibility of applying photometry from the 2MASS J, H, K

Cited by 5 publications

References 15 publications

3D structure of HII region Sh2-235 from tunable-filter optical observations

3D structure of HII region Sh2-235 from tunable-filter optical observations

Towards a census of the Galactic anticentre star clusters - II. Exploring lower overdensities

Open clusters in Auriga OB2

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