The distances and dimensions of IC 1805, IC 1848, and IC 410.

Sharpless, S.

doi:10.1086/107207

Cited by 4 publications

(6 citation statements)

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“…The distance derivations of previous investigators ranged from 1.7 kpc to 2.4 kpc. Sharpless (1955) obtained a distance of 1.7 kpc from their spectral types and photometric data for O stars. However, the author did not discuss the treatment of extinction correction nor considered binarity.…”

Section: Distance To Ic 1848mentioning

confidence: 99%

“…Several photometric studies (Sharpless 1955;Johnson et al 1961;Hoag et al 1961;Becker & Fenkart 1971;Moffat 1972;Loktin et al 2001) involving IC 1848 have been made in the optical bands. These studies provided useful photometric data and fundamental parameters, such as reddening, distance, and age for IC 1848.…”

Section: Introductionmentioning

confidence: 99%

“…The previously published distance to IC 1848, derived using various methods, is in the range 1.7 to 2.4 kpc. The photometric surveys mentioned above provided distances of 1.7 kpc (Sharpless 1955), 2.1±0.3 kpc (Chauhan et al 2011), 2.2 ± 0.2 kpc (Johnson et al 1961;Loktin et al 2001), and 2.3 kpc (Moffat 1972;Becker & Fenkart 1971). Some studies have implicitly assumed that the distance to IC 1848 is the same as that to W3 or W4 (or IC 1805) (1.9 -2.4 kpc).…”

Section: Introductionmentioning

confidence: 99%

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Sejong Open Cluster Survey (SOS) – II. IC 1848 cluster in the H ii region W5 West

Lim

Sung

Kim

et al. 2013

Monthly Notices of the Royal Astronomical Society

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IC 1848 is one of the young open clusters in the giant star forming Cas OB6 association. Several interesting aspects relating to star formation processes in giant star forming regions attracted us to study the initial mass function (IMF), star formation mode, and properties of pre-main sequence stars (PMS). A U BV I and Hα photometric study of the young open cluster IC 1848 was conducted as part of the "Sejong Open cluster Survey" (SOS). We have selected 105 early-type members from photometric diagrams. Their mean reddening is E(B − V ) = 0.660 ± 0.054 mag. Using the published photometric data with near-and mid-infrared archival data we confirmed the normal reddening law (R V = 3.1) toward the cluster (IC 1848). A careful zero-age main sequence fitting gives a distance modulus of V 0 − M V = 11.7 ± 0.2 mag, equivalent to 2.2 ± 0.2 kpc. Hα photometry and the list of young stellar objects identified by Koenig et al. permitted us to select a large number of PMS stars comprising 196 Hα emission stars, 35 Hα emission candidates, 5 Class I, 368 Class II, and 24 transition disk candidates. From the Hertzsprung-Russell diagram using stellar evolution models, we estimate an age of 5 Myr from several evolved stars and 3 Myr from the PMS stars. The IMF was derived from stars with mass larger than 3M , and the slope is slightly steeper (Γ = −1.6 ± 0.2) than the Salpeter/Kroupa IMF. Finally, we estimated the mass accretion rate of PMS stars with a UV excess. The mean mass accretion rate is about 1.4 × 10 −8 M yr −1 in the mass range of 0.5M to 2M , whereas intermediate-mass stars ( 2.5M ) exhibit a much higher accretion rate oḟ M > 10 −6 M yr −1 .

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Section: Distance To Ic 1848mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Sejong Open Cluster Survey (SOS) – II. IC 1848 cluster in the H ii region W5 West

Lim

Sung

Kim

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…The massive star-forming region (SFR) W5, which is a major part of the Cassiopeia OB6 association, is an ideal target in which to study the formation process of stellar associations. The previously determined distances to this SFR range from 1.7 to 2.3 kpc (Sharpless 1955;Johnson et al 1961;Becker & Fenkart 1971;Moffat 1972;Georgelin & Georgelin 1976;Loktin et al 2001;Chauhan et al 2011;Lim et al 2014a). Its age is younger than 5 Myr (Karr & Martin 2003;Koenig & Allen 2011;Lim et al 2014a).…”

Section: Introductionmentioning

confidence: 80%

The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations

Lim

Lee

Yun

et al. 2023

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The star-forming region W5 is a major part of the Cassiopeia OB6 association. Its internal structure and kinematics may provide hints of the star formation process in this region. Here, we present a kinematic study of young stars in W5 using the Gaia data and our radial velocity data. A total 490 out of 2000 young stars are confirmed as members. Their spatial distribution shows that W5 is highly substructured. We identify a total of eight groups using the k-means clustering algorithm. There are three dense groups in the cavities of H ii bubbles, and the other five sparse groups are distributed at the edges of the bubbles. The three dense groups have almost the same age (5 Myr) and show a pattern of expansion. The scale of their expansion is not large enough to account for the overall structure of W5. The three northern groups are, in fact, 3 Myr younger than the dense groups, which indicates independent star formation events. Only one of these groups shows the signature of feedback-driven star formation as its members move away from the eastern dense group. The other two groups might have formed in a spontaneous way. On the other hand, the properties of two southern groups are not understood as those of a coeval population. Their origins can be explained by dynamical ejection of stars and multiple star formation. Our results suggest that the substructures in W5 formed through multiple star-forming events in a giant molecular cloud.

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“…The bright rim type of this cloud was classified as type B (tightly curved rim; Sugitani et al 1991) based on its optical shape. The distance range of W5 in the literature is 1.7-2.3 kpc (Sharpless 1955;Johnson et al 1961;Ishida 1970;Georgelin & Georgelin 1976;Chauhan et al 2011). In this paper, we adopt the most recent value of 2.2 kpc for the open cluster IC1848 (Lim et al 2014) as the distance to SFO12 and its exciting stars in W5-W. Four O stars (BD +60 586 A, HD 237019, HD 17520 and HD 17505; Koenig et al 2008) are present in the W5-W and the main exciting star of the bright rim of SFO 12 is BD +60 586 A (O7V; Sota et al 2011), as seen in Figure 1.…”

Section: Introductionmentioning

confidence: 99%

High-resolution Near-infrared Observations of a Small Cluster Associated with a Bright-rimmed Cloud in W5

Imai

Sugitani

Miao

et al. 2017

ApJ

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We have carried out near-infrared (IR) observations to examine star formation toward the bright-rimmed cloud SFO 12, of which the main exciting star is O7V star in W5-W. We found a small young stellar object (YSO) cluster of six members embedded in the head of SFO 12 facing its exciting star, aligned along the UV radiation incident direction from the exciting star. We carried out high-resolution near-IR observations with the Subaru adaptive optics (AO) system and revealed that three of the cluster members appear to have circumstellar envelopes, one shows an arm-like structure in its envelope. Our near-IR and L ′ -band photometry and Spitzer IRAC data suggest that formation of two members at the tip side occurred in advance of other members toward the central part, under our adopted assumptions. Our near-IR data and previous 2 studies imply that more YSOs are distributed in the region just outside the cloud head on the side of the main exciting star, but there is little sign of star formation toward the opposite side. We infer that star formation has been sequentially occurring from the exciting star side to the central part. We examined archival data of far-infrared and CO (J = 3-2) which reveals that, unlike in the optical image, SFO 12 has a headtail structure which is along the UV incident direction. This suggests that SFO 12 is affected by strong UV from the main exciting star. We discuss the formation of this head-tail structure and star formation there by comparing with a radiation-driven implosion (RDI) model.

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The distances and dimensions of IC 1805, IC 1848, and IC 410.

Cited by 4 publications

References 0 publications

Sejong Open Cluster Survey (SOS) – II. IC 1848 cluster in the H ii region W5 West

Sejong Open Cluster Survey (SOS) – II. IC 1848 cluster in the H ii region W5 West

The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations

High-resolution Near-infrared Observations of a Small Cluster Associated with a Bright-rimmed Cloud in W5

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