E. Nikogossian - Academia.edu (original) (raw)

Papers by E. Nikogossian

Research paper thumbnail of PMS objects in the star formation region Cep OB3. II. Young stellar objects in the Hα nebula Cep B

Astrophysics, 2013

Models for the spectral energy distributions of four stellar objects in the bright compact Hα neb... more Models for the spectral energy distributions of four stellar objects in the bright compact Hα nebula Cep B are constructed. With a high probability, three of them are found to be very young stellar objects of evolutionary class 0/I with ages of 10 4-10 5 years, comparable to the kinematic age of the ionization front of the nebula itself. The IRAS 22551+6221 source associated with Cep B is initiated by heated dust. An intermediate-mass (B2-B3) star of evolutionary class III lies at the center of the ionization front. The local density of PMS stars in the immediate neighborhood of the Cep B nebula exceeds that for the cluster as a whole. It is highly probable that this zone is a local source of a new star-formation stage.

Research paper thumbnail of Luminosity Function for Quasars: Samples from Areas of the Clusters of Galaxies

Highlights of Spanish Astrophysics II, 2001

Research paper thumbnail of Search for HH-Objects and Emission-Line Stars in Star Forming Regions. I. The Lynds 1340 Dark Cloud

Spectroscopic and photometric observations of objects embedded in the L1340 dark cloud are report... more Spectroscopic and photometric observations of objects embedded in the L1340 dark cloud are reported. An entire series of HH-objects in the RN07 region was discovered, including new ones that form two or three flows. It is suspected that several cases of HH emission are included. In addition, 14 emission stars, of which 11 are new, were found in this region. Most of these stars are localized inside the RN07 nebula which, therefore, encompasses a compact cluster of very young stars. Other nebulous objects inside the L1340 cloud, many of which are associated with IR sources, are described. As a whole, this cloud represents an extremely active star forming region.

Research paper thumbnail of Structure of the Clusters of Galaxies A 2634, A 1983, and DC 0428-53

The hierarchical and dynamical structure of three clusters of galaxies, A 2634, A 1983, and DC 04... more The hierarchical and dynamical structure of three clusters of galaxies, A 2634, A 1983, and DC 042853, is investigated. Based on their example, we can say that the central cD galaxies play the leading role in clusters, affecting the course of their evolution. Radio and x-ray galaxies are not always part of the substructure. The morphological composition of various hierarchical subgroups depends on the stage of evolution. Clusters have a tendency to be oriented in the direction toward the nearest neighbor.

Research paper thumbnail of Structure of the clusters of galaxies a 999, a 1016, and a 1142

Astrophysics, 2000

ABSTRACT

Research paper thumbnail of PMS-objects in the star formation region Cep OB3. I. Stars with Hα emission

Astrophysics, 2013

ABSTRACT Results are presented from a detailed analysis of PMS stars located in the star-formatio... more ABSTRACT Results are presented from a detailed analysis of PMS stars located in the star-formation region that includes the bright part of the ionization front of the molecular cloud Cep B. Slitless spectroscopy is used to detect 149 stars with Ha emission. Models for the distribution of the spectral energy are constructed for 203 PMS stars based on photometric data in the visible and infrared and their basic parameters are determined. A good correlation is observed between the Hα emission intensity and the infrared excess. The relative disk mass and degree of accretion for stars with EW(Hα) > 10Å and α > −1.8 are about an order of magnitude greater than for the other stellar objects. The average distance and age of the PMS stars in the cluster are 890 pc and 0.74 million years, respectively. The stars with EW(Hα) > 10Å and α > −1.8 are more than 0.5 million years “younger” than the others.

Research paper thumbnail of New HH objects in star-forming regions: Parsec-scale outflows in GM 2–30

Astronomy Reports, 2007

We examine the star-forming region in a molecular cloud with the coordinates l = 33.30 • , b = 0.... more We examine the star-forming region in a molecular cloud with the coordinates l = 33.30 • , b = 0.25 • at a distance of 1.7 kpc, in which the nebula GM 2-30 is embedded. Apart from the previously known Herbig-Haro object HH 172, several new HH objects have been found, comprising at least two HH flows. The internal structure of these objects is studied. The relationship between the line emission and kinematic data obtained through multi-pupil spectroscopy suggest the presence of bipolar outflow associated with the nebula GM 2-30 and HH 172/HH 721, which show mirror symmetry according to a number of characteristics. No optical source of this flow is observed, although the source of energy of the second flow may be a weak star associated with HH 723. The linear dimensions of the flows (more than one parsec) suggest that they are the giant outflows.

Research paper thumbnail of Some questions on the structural properties of the Coma cluster

Research paper thumbnail of Narrow band imaging survey of outflows and reflection nebulae in compact star forming region

Research paper thumbnail of New Herbig-Haro Objects and Halpha Emission Stars in the Star Forming Regions GM 1-64/GM 2-4 and GM 2-41

Research paper thumbnail of 2D Spectroscopy of HH588 Large-Scale Outflow

The HH588 flow is studied with multi-pupil spectrograph on the 2.6 m telescope of Byurakan observ... more The HH588 flow is studied with multi-pupil spectrograph on the 2.6 m telescope of Byurakan observatory. The bright components of this flow are analyzed, using the maps of emission lines and radial velocities. The bipolar nature of this outflow is obvious from their radial velocities. The unusual feature of HH588 flow is its inclusion in the bright-rimmed cloud; thus, it can belong to so-called irradiated jets. It is worth to mention that all HH-objects studied here show a deceleration in the regions of interaction with the interstellar medium.

Research paper thumbnail of The Multiple Systems in The Young Stellar Cluster located in the vicinity of IRAS 05137+3919 source

Four binary objects and one triplet have been revealed in the young stellar cluster located in th... more Four binary objects and one triplet have been revealed in the young stellar cluster located in the vicinity of IRAS 05137+3919 source on a distance 4.4 kpc with the use of statistic analysis (2PCF, Poisson statistic). They are including the pair of AeBe stars. The percentage of the multiple systems in the cluster is mf = 5 and cp = 10.It should be noticed, that the use of the different databases, namely 2MASS and GPS UKIDSS, which are differ by both photometric limit and resolution, do not affect the value of these parameters. The mass of the multiple systems' components are located in the range from 1 to 8 Msol and log P (rotation period in years) - from 4.4 to 4.7. The median value of the mass ratio of the components is q = 0.73. The percentage of the multiple systems and their parameters in this cluster is resembling with the data obtained in the other star forming regions (ONC, Perseus, U Sco A), in which the value of mf and cp parameters are comparable with the results obta...

Research paper thumbnail of The search of the stellar clusters in vicinity of YSOs with high and middle masses

The results of the searching on the bases of GPS UKIDSS survey's data of dense compact stella... more The results of the searching on the bases of GPS UKIDSS survey's data of dense compact stellar clusters in the vicinity of 19 YSOs with high and middle masses are presented. Totally we have revealed clusters in 12 areas. Around 5 objects (IRAS 18151-1208, IRAS 18316-0602, IRAS 19110+1045, IRAS 19213+1723, IRAS 20056+3350) they are newly detected. The clusters associated with IRAS 05168+3634, IRAS 20188+3928, IRAS 19374+2352 and IRAS 19388+2357 sources have been already revealed on the less depth data than GPS UKIDSS survey images. The compact groups of stars located in the vicinity of IRAS 05358+3543, IRAS 18507+0121 and IRAS 20198+3716 sources belong to the more extensive clusters. The radii and stellar density have significant gradient: from 0.2 to 2.7 pc and from 3 to 1000 stars/arcmin^2 respectively. In the vicinity of 7 IRAS sources (IRAS 18174-1612, IRAS 18360-0537, IRAS 18385-0512, IRAS 18517+0437, IRAS 19092+0841, IRAS 19410+2336, IRAS 20126+4104) the stellar clusters we...

Research paper thumbnail of Figure.8

The wide-field view of the region in H2 where offsets are measured from IRS4 and solid line box s... more The wide-field view of the region in H2 where offsets are measured from IRS4 and solid line box shows the area presented in Fig. 2(b).Overlaid contours are from AV map constructed from 2MASS PSC and provided by Rowles & Froebrich (2009). Filled circles indicate the positions of IRAC identified Class I/II YSO sources provided by Gutermuth et al. (2009) where the colour spans according to the range of IRAC SED Slope (Alpha^ IRAC).

Research paper thumbnail of Stellar rotation in h Per (Moraux+, 2013)

List of periodic objects ordered by periodogram peak power. The binary flag is set to 2 if the ob... more List of periodic objects ordered by periodogram peak power. The binary flag is set to 2 if the object has been identified as a binary in the i'CFHT, i'CFHT-K CMD and to 1 otherwise. The V and IC magnitudes as well as the membership flag (column before last) are from Currie et al. (2010, Cat. J/ApJS/186/191). The near infrared photometry has been obtained with WIRCam at CFHT and is from Cardoso et al. (in prep.). The last column indicates whether the object has been detected in Hα (Currie et al., 2007, Cat. J/ApJ/659/599) and/or in X-rays (Currie et al., 2009, Cat. J/AJ/137/3210; C. Argiroffi, priv. com). (1 data file).

Research paper thumbnail of Figure.4

Close-up view in H2 1-0 S(1) emission of the area surrounding the IRAS 05373+2349 and the near-in... more Close-up view in H2 1-0 S(1) emission of the area surrounding the IRAS 05373+2349 and the near-infrared cluster where numerous MHOs where identified. Positions of IRS4 and 5 are marked with crosses on all panels. Panel (a) reveals details of MHO 734, 739, 740, 744 and 745. Panel (b) shows the suggested outflow structure with dotted arrows. Overlaid contours are from the 3.6cm emission starting from 3� and climbing with a 3� step-size and are from the data published by Molinari et al. (2002). Positions of 3.6cm peaks are marked with CM-A, -B and -C.

Research paper thumbnail of Figure.5

Scaled-up views of MHO 738 and 741 where the offsets are calculated from IRS4. Dotted-line arrows... more Scaled-up views of MHO 738 and 741 where the offsets are calculated from IRS4. Dotted-line arrows show the direction of the suggested bipolar outflow. Panel (a) shows the area including MHO 741 in H2 1-0 S(1) emission and the panel (b) is the same area in Spitzer IRAC composite view constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands. Panel (c) and panel (d) show the same wavelengths as in panels (a) and (b) but for the area including the MHO 738A, B and C.

Research paper thumbnail of Figure.2

Close-up view of GM 2-4 and IRAS 05373+2349 including the region where new molecular hydrogen emi... more Close-up view of GM 2-4 and IRAS 05373+2349 including the region where new molecular hydrogen emission line objects (MHOs) are found. Class I sources reported by Gutermuth et al. (2009) are marked with a crosses on all panels. Panel (a) is optical [SII] image where Herbig-Haro objects discovered by (Nikogossian et al. 2009) are marked along with the GM 2-4, GGD 4a and IRAS 05373+2349 error ellipse. Panel (b) is near-infrared H2 1-0 S(1) line+continuum image where the MHOs are marked with squares. Panel (c) shows Spitzer IRAC colour-composite image constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands with positions of newly detected MHOs marked with squares for a comparison. For this particular case the brightest (mostly saturated) stars in the field were truncated in order to stretch the colour scheme and reveal relatively fainter objects.

Research paper thumbnail of Figure.7

Spectral energy distribution (SED) of IRS3 to IRS7. Filled circles are the data points and the tr... more Spectral energy distribution (SED) of IRS3 to IRS7. Filled circles are the data points and the triangles are lower and upper limits where errors are generally smaller than the data points. The solid black line indicates the best-fitting model, and the grey lines show all models that also fit the data satisfying the Chi^2 - Chi^2 best < 3 per data point criteria. The dashed line shows the SED of the assumed stellar photosphere in the best-fitting model.

Research paper thumbnail of Figure.1

General field including GM 1-64 and GM 2-4 centred on IRAS 05373+2349. Panel (a) is DSS2 red imag... more General field including GM 1-64 and GM 2-4 centred on IRAS 05373+2349. Panel (a) is DSS2 red image of the region overlaid with a visual extinction contours obtained from Dobashi et al. (2005) peaking at TGU H1314. The solid-line ellipse indicates the positional uncertainty of IRAS 05373+2349 and the green asterisks mark the positions of masers. Panel (b) is the 2MASS false colour composite view of the region constructed from J (blue), H (green) and Ks (red) bands. Overlaid are the IRAS 100�m contours at 50, 70, 90 and 110 MJy/sterad. Panel (c) is Spitzer IRAC colour composite image constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands. Stars marked with big and small circles are sources reported by Gutermuth et al. (2009) and classified as Class I protostars and Class II pre-main-sequence stars respectively. Panel (d) is Spitzer MIPS 24�m band view of the region where the same Class I sources are marked with the nomenclature used in our study.

Research paper thumbnail of PMS objects in the star formation region Cep OB3. II. Young stellar objects in the Hα nebula Cep B

Astrophysics, 2013

Models for the spectral energy distributions of four stellar objects in the bright compact Hα neb... more Models for the spectral energy distributions of four stellar objects in the bright compact Hα nebula Cep B are constructed. With a high probability, three of them are found to be very young stellar objects of evolutionary class 0/I with ages of 10 4-10 5 years, comparable to the kinematic age of the ionization front of the nebula itself. The IRAS 22551+6221 source associated with Cep B is initiated by heated dust. An intermediate-mass (B2-B3) star of evolutionary class III lies at the center of the ionization front. The local density of PMS stars in the immediate neighborhood of the Cep B nebula exceeds that for the cluster as a whole. It is highly probable that this zone is a local source of a new star-formation stage.

Research paper thumbnail of Luminosity Function for Quasars: Samples from Areas of the Clusters of Galaxies

Highlights of Spanish Astrophysics II, 2001

Research paper thumbnail of Search for HH-Objects and Emission-Line Stars in Star Forming Regions. I. The Lynds 1340 Dark Cloud

Spectroscopic and photometric observations of objects embedded in the L1340 dark cloud are report... more Spectroscopic and photometric observations of objects embedded in the L1340 dark cloud are reported. An entire series of HH-objects in the RN07 region was discovered, including new ones that form two or three flows. It is suspected that several cases of HH emission are included. In addition, 14 emission stars, of which 11 are new, were found in this region. Most of these stars are localized inside the RN07 nebula which, therefore, encompasses a compact cluster of very young stars. Other nebulous objects inside the L1340 cloud, many of which are associated with IR sources, are described. As a whole, this cloud represents an extremely active star forming region.

Research paper thumbnail of Structure of the Clusters of Galaxies A 2634, A 1983, and DC 0428-53

The hierarchical and dynamical structure of three clusters of galaxies, A 2634, A 1983, and DC 04... more The hierarchical and dynamical structure of three clusters of galaxies, A 2634, A 1983, and DC 042853, is investigated. Based on their example, we can say that the central cD galaxies play the leading role in clusters, affecting the course of their evolution. Radio and x-ray galaxies are not always part of the substructure. The morphological composition of various hierarchical subgroups depends on the stage of evolution. Clusters have a tendency to be oriented in the direction toward the nearest neighbor.

Research paper thumbnail of Structure of the clusters of galaxies a 999, a 1016, and a 1142

Astrophysics, 2000

ABSTRACT

Research paper thumbnail of PMS-objects in the star formation region Cep OB3. I. Stars with Hα emission

Astrophysics, 2013

ABSTRACT Results are presented from a detailed analysis of PMS stars located in the star-formatio... more ABSTRACT Results are presented from a detailed analysis of PMS stars located in the star-formation region that includes the bright part of the ionization front of the molecular cloud Cep B. Slitless spectroscopy is used to detect 149 stars with Ha emission. Models for the distribution of the spectral energy are constructed for 203 PMS stars based on photometric data in the visible and infrared and their basic parameters are determined. A good correlation is observed between the Hα emission intensity and the infrared excess. The relative disk mass and degree of accretion for stars with EW(Hα) &gt; 10Å and α &gt; −1.8 are about an order of magnitude greater than for the other stellar objects. The average distance and age of the PMS stars in the cluster are 890 pc and 0.74 million years, respectively. The stars with EW(Hα) &gt; 10Å and α &gt; −1.8 are more than 0.5 million years “younger” than the others.

Research paper thumbnail of New HH objects in star-forming regions: Parsec-scale outflows in GM 2–30

Astronomy Reports, 2007

We examine the star-forming region in a molecular cloud with the coordinates l = 33.30 • , b = 0.... more We examine the star-forming region in a molecular cloud with the coordinates l = 33.30 • , b = 0.25 • at a distance of 1.7 kpc, in which the nebula GM 2-30 is embedded. Apart from the previously known Herbig-Haro object HH 172, several new HH objects have been found, comprising at least two HH flows. The internal structure of these objects is studied. The relationship between the line emission and kinematic data obtained through multi-pupil spectroscopy suggest the presence of bipolar outflow associated with the nebula GM 2-30 and HH 172/HH 721, which show mirror symmetry according to a number of characteristics. No optical source of this flow is observed, although the source of energy of the second flow may be a weak star associated with HH 723. The linear dimensions of the flows (more than one parsec) suggest that they are the giant outflows.

Research paper thumbnail of Some questions on the structural properties of the Coma cluster

Research paper thumbnail of Narrow band imaging survey of outflows and reflection nebulae in compact star forming region

Research paper thumbnail of New Herbig-Haro Objects and Halpha Emission Stars in the Star Forming Regions GM 1-64/GM 2-4 and GM 2-41

Research paper thumbnail of 2D Spectroscopy of HH588 Large-Scale Outflow

The HH588 flow is studied with multi-pupil spectrograph on the 2.6 m telescope of Byurakan observ... more The HH588 flow is studied with multi-pupil spectrograph on the 2.6 m telescope of Byurakan observatory. The bright components of this flow are analyzed, using the maps of emission lines and radial velocities. The bipolar nature of this outflow is obvious from their radial velocities. The unusual feature of HH588 flow is its inclusion in the bright-rimmed cloud; thus, it can belong to so-called irradiated jets. It is worth to mention that all HH-objects studied here show a deceleration in the regions of interaction with the interstellar medium.

Research paper thumbnail of The Multiple Systems in The Young Stellar Cluster located in the vicinity of IRAS 05137+3919 source

Four binary objects and one triplet have been revealed in the young stellar cluster located in th... more Four binary objects and one triplet have been revealed in the young stellar cluster located in the vicinity of IRAS 05137+3919 source on a distance 4.4 kpc with the use of statistic analysis (2PCF, Poisson statistic). They are including the pair of AeBe stars. The percentage of the multiple systems in the cluster is mf = 5 and cp = 10.It should be noticed, that the use of the different databases, namely 2MASS and GPS UKIDSS, which are differ by both photometric limit and resolution, do not affect the value of these parameters. The mass of the multiple systems' components are located in the range from 1 to 8 Msol and log P (rotation period in years) - from 4.4 to 4.7. The median value of the mass ratio of the components is q = 0.73. The percentage of the multiple systems and their parameters in this cluster is resembling with the data obtained in the other star forming regions (ONC, Perseus, U Sco A), in which the value of mf and cp parameters are comparable with the results obta...

Research paper thumbnail of The search of the stellar clusters in vicinity of YSOs with high and middle masses

The results of the searching on the bases of GPS UKIDSS survey's data of dense compact stella... more The results of the searching on the bases of GPS UKIDSS survey's data of dense compact stellar clusters in the vicinity of 19 YSOs with high and middle masses are presented. Totally we have revealed clusters in 12 areas. Around 5 objects (IRAS 18151-1208, IRAS 18316-0602, IRAS 19110+1045, IRAS 19213+1723, IRAS 20056+3350) they are newly detected. The clusters associated with IRAS 05168+3634, IRAS 20188+3928, IRAS 19374+2352 and IRAS 19388+2357 sources have been already revealed on the less depth data than GPS UKIDSS survey images. The compact groups of stars located in the vicinity of IRAS 05358+3543, IRAS 18507+0121 and IRAS 20198+3716 sources belong to the more extensive clusters. The radii and stellar density have significant gradient: from 0.2 to 2.7 pc and from 3 to 1000 stars/arcmin^2 respectively. In the vicinity of 7 IRAS sources (IRAS 18174-1612, IRAS 18360-0537, IRAS 18385-0512, IRAS 18517+0437, IRAS 19092+0841, IRAS 19410+2336, IRAS 20126+4104) the stellar clusters we...

Research paper thumbnail of Figure.8

The wide-field view of the region in H2 where offsets are measured from IRS4 and solid line box s... more The wide-field view of the region in H2 where offsets are measured from IRS4 and solid line box shows the area presented in Fig. 2(b).Overlaid contours are from AV map constructed from 2MASS PSC and provided by Rowles & Froebrich (2009). Filled circles indicate the positions of IRAC identified Class I/II YSO sources provided by Gutermuth et al. (2009) where the colour spans according to the range of IRAC SED Slope (Alpha^ IRAC).

Research paper thumbnail of Stellar rotation in h Per (Moraux+, 2013)

List of periodic objects ordered by periodogram peak power. The binary flag is set to 2 if the ob... more List of periodic objects ordered by periodogram peak power. The binary flag is set to 2 if the object has been identified as a binary in the i'CFHT, i'CFHT-K CMD and to 1 otherwise. The V and IC magnitudes as well as the membership flag (column before last) are from Currie et al. (2010, Cat. J/ApJS/186/191). The near infrared photometry has been obtained with WIRCam at CFHT and is from Cardoso et al. (in prep.). The last column indicates whether the object has been detected in Hα (Currie et al., 2007, Cat. J/ApJ/659/599) and/or in X-rays (Currie et al., 2009, Cat. J/AJ/137/3210; C. Argiroffi, priv. com). (1 data file).

Research paper thumbnail of Figure.4

Close-up view in H2 1-0 S(1) emission of the area surrounding the IRAS 05373+2349 and the near-in... more Close-up view in H2 1-0 S(1) emission of the area surrounding the IRAS 05373+2349 and the near-infrared cluster where numerous MHOs where identified. Positions of IRS4 and 5 are marked with crosses on all panels. Panel (a) reveals details of MHO 734, 739, 740, 744 and 745. Panel (b) shows the suggested outflow structure with dotted arrows. Overlaid contours are from the 3.6cm emission starting from 3� and climbing with a 3� step-size and are from the data published by Molinari et al. (2002). Positions of 3.6cm peaks are marked with CM-A, -B and -C.

Research paper thumbnail of Figure.5

Scaled-up views of MHO 738 and 741 where the offsets are calculated from IRS4. Dotted-line arrows... more Scaled-up views of MHO 738 and 741 where the offsets are calculated from IRS4. Dotted-line arrows show the direction of the suggested bipolar outflow. Panel (a) shows the area including MHO 741 in H2 1-0 S(1) emission and the panel (b) is the same area in Spitzer IRAC composite view constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands. Panel (c) and panel (d) show the same wavelengths as in panels (a) and (b) but for the area including the MHO 738A, B and C.

Research paper thumbnail of Figure.2

Close-up view of GM 2-4 and IRAS 05373+2349 including the region where new molecular hydrogen emi... more Close-up view of GM 2-4 and IRAS 05373+2349 including the region where new molecular hydrogen emission line objects (MHOs) are found. Class I sources reported by Gutermuth et al. (2009) are marked with a crosses on all panels. Panel (a) is optical [SII] image where Herbig-Haro objects discovered by (Nikogossian et al. 2009) are marked along with the GM 2-4, GGD 4a and IRAS 05373+2349 error ellipse. Panel (b) is near-infrared H2 1-0 S(1) line+continuum image where the MHOs are marked with squares. Panel (c) shows Spitzer IRAC colour-composite image constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands with positions of newly detected MHOs marked with squares for a comparison. For this particular case the brightest (mostly saturated) stars in the field were truncated in order to stretch the colour scheme and reveal relatively fainter objects.

Research paper thumbnail of Figure.7

Spectral energy distribution (SED) of IRS3 to IRS7. Filled circles are the data points and the tr... more Spectral energy distribution (SED) of IRS3 to IRS7. Filled circles are the data points and the triangles are lower and upper limits where errors are generally smaller than the data points. The solid black line indicates the best-fitting model, and the grey lines show all models that also fit the data satisfying the Chi^2 - Chi^2 best < 3 per data point criteria. The dashed line shows the SED of the assumed stellar photosphere in the best-fitting model.

Research paper thumbnail of Figure.1

General field including GM 1-64 and GM 2-4 centred on IRAS 05373+2349. Panel (a) is DSS2 red imag... more General field including GM 1-64 and GM 2-4 centred on IRAS 05373+2349. Panel (a) is DSS2 red image of the region overlaid with a visual extinction contours obtained from Dobashi et al. (2005) peaking at TGU H1314. The solid-line ellipse indicates the positional uncertainty of IRAS 05373+2349 and the green asterisks mark the positions of masers. Panel (b) is the 2MASS false colour composite view of the region constructed from J (blue), H (green) and Ks (red) bands. Overlaid are the IRAS 100�m contours at 50, 70, 90 and 110 MJy/sterad. Panel (c) is Spitzer IRAC colour composite image constructed from 3.6�m (blue), 4.5�m (green) and 8.0�m (red) bands. Stars marked with big and small circles are sources reported by Gutermuth et al. (2009) and classified as Class I protostars and Class II pre-main-sequence stars respectively. Panel (d) is Spitzer MIPS 24�m band view of the region where the same Class I sources are marked with the nomenclature used in our study.