clump are dominated by protostar emission despite the contamination by
extended shock structures. The 2MASS census is also biased by the emission of
warm H2, as the band K ($\lambda$=2.159 $\upmu$m, $\Delta\lambda$=0.262
$\upmu$m) is sensitive to the rovibrational line $\varv=1-0$ S(1) at 2.12
$\upmu$m. The clumpy and bright extended emission displayed in the band K map
of the southern ridge makes it clear that the flux of point sources might be
contaminated by extended emission, in particular along the bright shocked
clump. Rho et al. (2001) confirmed that the band K extended emission from this
region of the remnant is dominated by H2 emission, and to a lesser extent the
bands J and H. On the one hand, if the flux of the band K is overestimated due
to H2 emission, then the correction would lead to a displacement along the H-K
axis, which means that more protostar candidates would be detected towards the
shocked clump where the emission of warm H2 is significant. This might explain
why the higher density of protostar candidates found in the WISE census is not
reproduced by our 2MASS census. On the other hand, it is possible that a
number of point sources detected by 2MASS are unresolved knots of shocked H2,
in a similar fashion as what is expected for WISE.

A greater amount of point sources is found on the edges of the 24$\upmu$m
bright knot that is spatially associated with the eastern edge of the
quiescent molecular cloudlet. Excluding the shocked clump, there is an anti-
correlation between both 2MASS and WISE sources and the MIPS-24$\upmu$m flux
map, in particular in the vicinity of the cloudlet. We suppose that the
absence of optical point sources within this region is due to the extinction
caused by this massive dark cloud. No IR point sources are found at the center
of the gap within the ring-like structure.

Interestingly, the few point sources that were not flagged for contamination
by extended sources are primarily organized in two clusters in the eastern and
north-eastern part of the field (group 1 and group 2, Fig. 14). All these
candidates were positively identified by both methods as Class I and Class II
protostars. The Class I protostar candidates of group 2 are well associated
with Spitzer-IRAC filamentary structures at 4.5 $\upmu$m, at the edge of a
faint structure detected by Spitzer-MIPS at 24 $\upmu$m. This bright filament
can be either part of the SNR shock or unresolved outflows. Most IR sources
with protostar signatures are spatially correlated with the molecular shell in
IC443G, suggesting enhanced star formation along the rims. Given the
protostellar collapse phase timescale of $\sim$105 yr (Lefloch & Lazareff,
1994) we dot not establish any causal relation between the SNR shocks and the
formation of Class I and Class II protostars. Based on our color-color census
for the 65 protostar candidates detected by WISE, the Class II / Class I ratio
is equal to 0.23. Following Dunham et al. (2015), we assumed a Class II
duration of 2 Myr and used the standard method to infer the age of a stellar
population from this ratio (Wilking et al. 1989, Evans et al. 2009). We obtain
an age of $\sim$500 kyr for the YSO population found in the extended G region,
which is not consistent with the scenario in which the formation of these YSOs
was triggered by interaction of the SNR with its environment. It is likely
that the collapse of molecular clouds in the vicinity of the high-mass
progenitor was triggered by the compression driven by stellar winds (Xu et
al., 2011). To find evidence of enhanced star formation in the SNR shocks
would require to detect deeply embedded prestellar cores, which is not
attainable with the data at our disposal. In the future, high-resolution
($\sim$1′′) sub-mm and mm observations will be required to disentangle the
kinematics of large-scale shock structure and outflows, and to eventually
uncover prestellar cores in the extended G region (e.g. as Motte et al. (2018)
did for the W43-MM1 star forming region). Still, our sample of protostar
candidates provides a unique opportunity to study star formation in an
environment that is subject to intense $\gamma$-ray flux and shock dynamical
feedback. The protons accelerated by young protostars might also provide a
source of fresh mid-energy CRs (up to 10-13 GeV and 26-37 GeV respectively for
jet acceleration and protostellar surface shock acceleration in lower-mass
stars, Padovani et al. 2016). With jet velocities up to 1000 km s-1, high-mass
protostellar shocks could contribute to the TeV $\gamma$-ray peak in the
extended G region.

Point sources identified as star-forming galaxies from their location in the
color-color diagram display a significant correlation with the spiral-shaped,
bright and extended infrared features mapped by Spitzer-MIPS at 24 $\upmu$m.
Most of these sources might as well be identified as PAH emission, as our
arbitrary criterion of selection puts a significant uncertainty on the cut
between the two categories of sources, in particular along the W1 \- W2 axis
(Koenig et al., 2012). In fact, it is more likely that these point sources are
associated with PAH, stellar or protostellar emission. With our current
criterion, only 2 sources identified as PAH emission are found and located in
the same area as point sources that were labelled ’star-forming galaxies’. If
most of these detections are actually arising from PAH emission, this result
would support the assumption that the bright infrared extended emission arise
from a dark dust lane that is spatially associated with the molecular cloudlet
detected by our CO observations.

In comparison to previous work on the star formation in IC443:

  * •

Based on 2MASS point source catalogues, Xu et al. (2011) found a total of 1666
YSO candidates, 154 CTTS and 419 HAeBe stars in a search circle around IC443
within a 25′ radius. Their candidates were mostly concentrated around the CO
molecular shell, in particular towards i. the clump C; ii. the extended G
region where their YSO candidates are spatially correlated with the shocked
clump. They proposed that the formation of these YSOs have been triggered by
the stellar wind of the IC443 progenitor.

  * •

Based on 2MASS and WISE point source catalogues, Su et al. (2014) found a
total of 98 YSO candidates. They proposed a sample of 62 YSO candidates
concentrated along the boundary of the radio shell. They also proposed that
the formation of these protostars is likely to have been triggered by the
stellar winds of the SNR progenitor. In contrast with our results and the
findings of Xu et al. (2011), their distribution does not show a strong
correlation with the molecular structures in the extended G region.

##  6 Summary

  1. 1.

In this work we report on new $10^{\prime}\times 10^{\prime}$ fully sampled
maps of the extended IC443G region for the first three rotational transitions
of both 12CO and 13CO, as well as the two first rotational transitions of C18O
obtained with the IRAM-30m and APEX telescope. These extensive maps allow to
probe the position of the TeV $\gamma$-ray peak in IC443G and its surroundings
with unprecedented spectral and angular resolution at millimeter and sub-
millimeter wavelengths.

  2. 2.

We proposed a description of the morphology and kinematics of the extended G
region based on the definition of four main molecular structures: (i.) a
shocked clump; (ii.) a quiescent, ”ring-like” structure that might be
spurious; (iii.) a quiescent cloudlet that is spatially connected to the ring-
like structure and (iv.) a shocked knot.

  3. 3.

The comparison of our data histograms with modified LTE radiative transfer
models revealed enhanced 12CO J=2–1/1–0 and J=3–2/2–1 ratios towards the
shocked clump, in particular within the high-velocity wings of the emission
lines that are tracing warm CO (40 - 120 K). We provide a rough estimate of
the isotopic ratio based on the best match between modified LTE models and the
measured intensity of the 12CO, 13CO and C18O J=1–0 line.

  4. 4.

We measured the mass of the molecular gas in the extended G region using
pixel-per-pixel, channel-per-channel population diagrams corrected for optical
depth. We obtained a total molecular mass estimate of $\sim$230 $M_{\odot}$,
$\sim$90 $M_{\odot}$, $\sim$210 $M_{\odot}$ and $\sim$4 $M_{\odot}$
respectively for the cloudlet, ring-like structure, shocked clump and shocked
knot. We also measured a mass of $\sim$1100 $M_{\odot}$ for the ambient gas in
the [-6.5, -1.5] km s-1 $\varv_{\mathrm{LSR}}$ range. The estimate of the mass
depends on the adopted 12CO/13CO isotopic ratio, but it is established that a
total molecular mass 0.9-3.1$\times 10^{3}$ $M_{\odot}$ is available to
interact with CRs via pion-decay in the extended G region.

  5. 5.

We proposed a second estimate of the mass using the LVG assumption with a grid
of RADEX models. The $\chi^{2}$-minimization of the grid of models with
respect to data in each structure yields results that are in partial agreement
with the previous measurements, with an estimate that is systematically lower
than the LTE estimate, except for the mass measurements of the high-velocity
wings towards the shocked clump, which are higher by a factor $\sim$3 .

  6. 6.

We studied the spectral energy distribution of infrared and optical point
sources using the 2MASS, WISE and Gaia catalogues of point sources. Using
color-color diagrams we determined a sample of protostar candidates in the
extended G region. 144 protostar candidates are found in the region, and 16
stars are found in the Gaia census but it is worth to note that a large
fraction of these point sources are contaminated by extended emission (12.7%
for 2MASS, and 76.9% for WISE). Based on the spatial distribution of these
candidates, we propose three sites of possible star formation in IC443G
(groups 1 and 2 in Fig. 14, and the shocked clump). These protostars might
constitute a source of fresh CRs.

###### Acknowledgements.

This work was supported by the Programme National ”Physique et Chimie du
Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and
CNES. This publication is based on observations made with ESO Telescopes at
the Atacama Pathfinder EXperiment under programme M-0102.F-9508A-2018. This
work has made use of data from the European Space Agency (ESA) mission Gaia
(https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and
Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has
been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement. This research has made use
of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under contract with
the National Aeronautics and Space Administration. This publication makes use
of data products from the Wide-field Infrared Survey Explorer, which is a
joint project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. This publication makes use of
data products from the Two Micron All Sky Survey, which is a joint project of
the University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National Aeronautics
and Space Administration and the National Science Foundation. This research
made use of Astropy,999http://www.astropy.org a community-developed core
Python package for Astronomy (Astropy Collaboration et al., 2013, 2018). This
research has made use of NASA’s Astrophysics Data System. M.P. acknowledges
funding from the INAF PRIN-SKA 2017 program 1.05.01.88.04.

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##  Appendix A Coordinates of the boxes

Table 9: Coordinates of the vertices defining the boxes corresponding to dense cloudlet, ring-like structure and shocked clump (Fig. 6, Tab. 9). region | r.a. [J2000] | dec. [J2000]
---|---|---
| $6^{\mathrm{h}}16^{\mathrm{m}}37.0^{\mathrm{s}}$ | $+22^{\circ}40^{\prime}24.0^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}23.1^{\mathrm{s}}$ | $+22^{\circ}40^{\prime}24.0^{\prime\prime}$
dense cloudlet | $6^{\mathrm{h}}16^{\mathrm{m}}23.1^{\mathrm{s}}$ | $+22^{\circ}33^{\prime}39.8^{\prime\prime}$
(A) | $6^{\mathrm{h}}16^{\mathrm{m}}30.3^{\mathrm{s}}$ | $+22^{\circ}33^{\prime}39.8^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}30.3^{\mathrm{s}}$ | $+22^{\circ}36^{\prime}09.5^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}37.0^{\mathrm{s}}$ | $+22^{\circ}36^{\prime}09.5^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}41.2^{\mathrm{s}}$ | $+22^{\circ}36^{\prime}09.5^{\prime\prime}$
ring-like structure | $6^{\mathrm{h}}16^{\mathrm{m}}30.3^{\mathrm{s}}$ | $+22^{\circ}36^{\prime}09.5^{\prime\prime}$
(B) | $6^{\mathrm{h}}16^{\mathrm{m}}30.3^{\mathrm{s}}$ | $+22^{\circ}33^{\prime}39.8^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}41.2^{\mathrm{s}}$ | $+22^{\circ}33^{\prime}39.8^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}47.1^{\mathrm{s}}$ | $+22^{\circ}34^{\prime}30.7^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}40.2^{\mathrm{s}}$ | $+22^{\circ}34^{\prime}30.7^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}40.2^{\mathrm{s}}$ | $+22^{\circ}32^{\prime}32.4^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}33.8^{\mathrm{s}}$ | $+22^{\circ}32^{\prime}32.4^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}33.8^{\mathrm{s}}$ | $+22^{\circ}31^{\prime}30.7^{\prime\prime}$
shocked clump | $6^{\mathrm{h}}16^{\mathrm{m}}31.9^{\mathrm{s}}$ | $+22^{\circ}31^{\prime}30.7^{\prime\prime}$
(C) | $6^{\mathrm{h}}16^{\mathrm{m}}31.9^{\mathrm{s}}$ | $+22^{\circ}29^{\prime}36.6^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}44.7^{\mathrm{s}}$ | $+22^{\circ}29^{\prime}36.6^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}44.7^{\mathrm{s}}$ | $+22^{\circ}31^{\prime}06.4^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}46.2^{\mathrm{s}}$ | $+22^{\circ}31^{\prime}06.4^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}46.2^{\mathrm{s}}$ | $+22^{\circ}32^{\prime}21.3^{\prime\prime}$
| $6^{\mathrm{h}}16^{\mathrm{m}}47.1^{\mathrm{s}}$ | $+22^{\circ}32^{\prime}21.3^{\prime\prime}$

##  Appendix B Thermometry of absorption lines

Considering a transition between an upper level $u$ and a lower level $l$ ,
the extinction coefficient $\kappa_{\nu}$ is given by:

$\kappa_{\nu}=\dfrac{c^{2}}{8\pi\nu_{ul}^{2}}A_{ul}n_{l}\dfrac{g_{u}}{g_{l}}\left[1-\mathrm{exp}\left(\dfrac{h\nu_{ul}}{kT_{ex}}\right)\right]\phi(\nu)$
(16)

Where $T_{ex}$ is the excitation temperature, $\phi(\nu)$ the profile of the
line , $\nu_{ul}$ the frequency of the transition, $A_{ul}$ the Einstein
coefficient of spontaneous emission, $n_{l}$ the density of the lower level
and $g_{u}$ and $g_{l}$ are the statistical weights. If $u\leftrightarrow J+1$
and $l\leftrightarrow J$, then the Einstein coefficient is defined by:

$A_{J+1\rightarrow
J}=\dfrac{64\pi^{4}\mu^{2}}{3hc^{3}}\dfrac{J+1}{2J+3}\nu_{J}^{3}$ (17)

Where $\mu$ is the dipole moment of the considered molecule. Thus, by using
this definition together with the definition of the statistical weights we
get:

$\kappa_{\nu}^{J\rightarrow
J+1}=\dfrac{8\pi^{3}\mu^{2}}{3hc}\dfrac{J+1}{2J+1}\nu_{J}n_{J}\left[1-\mathrm{exp}\left(-\dfrac{h\nu_{J}}{kT_{ex}}\right)\right]$
(18)

If we introduce the partition function we get a relation linking $n_{J}$ to
the total density $n$:

$n_{J}=n\dfrac{g_{J}}{Q(T_{ex})}\mathrm{exp}\left(-\dfrac{E_{J}}{kT_{ex}}\right)$
(19)

Where $E_{J}$ and $E_{J+1}$ are the level energies. So that:

$\kappa_{\nu}^{J\rightarrow
J+1}=\dfrac{8\pi^{3}\mu^{2}}{3hc}\nu_{J}n\dfrac{J+1}{Q(T_{ex})}\mathrm{exp}\left(-\dfrac{E_{J}}{kT_{ex}}\right)\left[1-\mathrm{exp}\left(\dfrac{E_{J}-E_{J+1}}{kT_{ex}}\right)\right]\phi(\nu)$
(20)

Thus the total column density $N$ can be obtained by computing the following
integral over the line of sight:

$\displaystyle N$ $\displaystyle=$ $\displaystyle\int\mathrm{d}s\int
n\phi(\nu)\mathrm{d}\nu$ $\displaystyle=$
$\displaystyle\int\mathrm{d}s\int\dfrac{\kappa_{\nu}^{J\rightarrow
J+1}\dfrac{3hc}{8\pi^{3}\mu^{2}}\dfrac{1}{\nu_{J}}\dfrac{Q(T_{ex})}{J+1}\mathrm{exp}\left(\dfrac{E_{J}}{kT_{ex}}\right)}{\left[1-\mathrm{exp}\left(\dfrac{E_{J}-E_{J+1}}{kT_{ex}}\right)\right]}\mathrm{d}\nu$

Using the definition of the equivalent width $W=\int\tau\mathrm{d}v$ and the
variable $\mathrm{d}\nu=\nu_{J}\mathrm{d}v/c$, we finally get the relation
between column density and equivalent width for a given excitation
temperature:

$N=\Lambda\dfrac{Q(T_{ex})}{1-\mathrm{exp}\left(\dfrac{-h\nu_{ij}}{kT_{ex}}\right)}W_{ij}$
(21)

Where $\Lambda=3h/8\pi^{3}\mu^{2}$, $h$ is the planck constant and $\nu_{ij}$
the frequency of the transition. Applied to the transitions J=1–0 and J=2–1,
this relation can be written for two different values of the equivalent width
$W$ corresponding to each line. As the total column density is constant in
each equation, the ratio of these two relations yields:

$1=\dfrac{1}{2}\mathrm{exp}\left(\dfrac{h\nu_{ij}}{kT_{ex}}\right)\dfrac{1-\mathrm{exp}\left(\dfrac{-h\nu_{ij}}{kT_{ex}}\right)}{1-\mathrm{exp}\left(\dfrac{-2h\nu_{ij}}{kT_{ex}}\right)}\dfrac{W_{1\rightarrow
2}}{W_{0\rightarrow 1}}$ (22)

If we define the temperature of the transition $T_{0}=h\nu_{ij}/k$ and use the
variable $u=T_{0}/T_{ex}$ then we have:

$2=\mathrm{e}^{2u}\dfrac{1-\mathrm{e}^{-2u}}{1-\mathrm{e}^{-4u}}\dfrac{W_{1\rightarrow
2}}{W_{0\rightarrow
1}}=\mathrm{e}^{3u}\dfrac{\mathrm{e}^{u}-\mathrm{e}^{-u}}{\mathrm{e}^{2u}-\mathrm{e}^{-2u}}\dfrac{W_{1\rightarrow
2}}{W_{0\rightarrow 1}}$ (23)

Or:

$2=\dfrac{\mathrm{e}^{3u}}{2\mathrm{cosh}(u)}\dfrac{W_{1\rightarrow
2}}{W_{0\rightarrow 1}}$ (24)

and, finally we get the following relation which permits to determine the
temperature from a measure of the ratio of the two equivalent widths:

$F\left(\dfrac{T_{0}}{T_{ex}}\right)=\dfrac{W_{1\rightarrow
2}}{4W_{0\rightarrow 1}}$ (25)

Where $F(u)=\mathrm{e}^{-3u}\mathrm{cosh}(u)$.

##  Appendix C Spatial distribution of YSO candidates

Figure 15: Spatial distribution of protostar candidates in our
10${}^{\prime}\times$10′ field of observations. Left: Class I and Class II
candidates detected by WISE. Right: YSO candidates detected by 2MASS. White
contours represent the CO(2-1) emission in the velocity range [-7, +3] km/s.

##  Appendix D Complementary channel maps

Figure 16: Channel map of the ${}^{12}\mathrm{CO}(1-0)$ observations carried
out with the IRAM-30m telescope. The $10^{\prime}\times 10^{\prime}$ field is
entirely displayed. Each panel represent the emission integrated over an
interval of $0.5\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$
around a given velocity along the line of sight. Velocities are indicated on
the top left corner of each panel. Velocity channels represented on this
figure are between $\varv=-20\leavevmode\nobreak\
\mathrm{km\leavevmode\nobreak\ s^{-1}}$ and $\varv=8\leavevmode\nobreak\
\mathrm{km\leavevmode\nobreak\ s^{-1}}$, covering all the spectral features
detected towards IC443G.

Figure 17: Channel map of the ${}^{13}\mathrm{CO}(1-0)$ observations carried
out with the IRAM-30m telescope. The $10^{\prime}\times 10^{\prime}$ field is
entirely displayed. Each panel represent the emission integrated over an
interval of velocity along the line of sight. Velocities are indicated on the
top left corner of each panel. Velocity channels represented in this figure
are between $\varv=-24\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\
s^{-1}}$ and $\varv=+12\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\
s^{-1}}$, covering all the spectral features detected towards the extended G
region.

Figure 18: Channel map of the ${}^{12}\mathrm{CO}(2-1)$ observations carried
out with the APEX. The $10^{\prime}\times 10^{\prime}$ field is entirely
displayed. Each panel represent the emission integrated over an interval of
velocity along the line of sight. Velocities are indicated on the top left
corner of each panel. Velocity channels represented in this figure are between
$\varv=-24\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$ and
$\varv=+12\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$,
covering all the spectral features detected towards the extended G region.

Figure 19: Channel map of the ${}^{12}\mathrm{CO}(3-2)$ observations carried
out with APEX. The $10^{\prime}\times 10^{\prime}$ field is entirely
displayed. Each panel represent the emission integrated over an interval of
velocity along the line of sight. Velocities are indicated on the top left
corner of each panel. Velocity channels represented in this figure are between
$\varv=-24\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$ and
$\varv=+12\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$,
covering all the spectral features detected towards the extended G region.

##  Appendix E Spectral energy distributions of protostar candidates

Figure 20: Spectral energy distributions of 17 protostar candidates. Their
corresponding ID in Tab. LABEL:table:2MASSphot and Tab. LABEL:table:WISEphot
ared indicated in the upper-left corner of each boxes when available (marked
with a ’*’ if not corresponding to any point sources identified by a label).
Red markers correspond to 2MASS photometric measures and black markers
correspond to WISE measures.

##  Appendix F Observational measure of the optical depth

Figure 21: Spectra obtained over the region of the four boxes defined in Fig.
6, for the following lines: ${}^{12}\mathrm{CO}$ (in black),
${}^{13}\mathrm{CO}$ (in blue) and $\mathrm{C^{18}O}$ (in red). First row
presents the (1–0) transition, second row presents the (2–1) transition and
third row presents the (3–2) transition for: A, the cloudlet; B, the ring-like
structure; C, the shocked clump and D, the shocked knot. Spectral cubes were
resampled to allow direct comparison between the different spectra. Spatial
resolutions of all transitions were modified to the nominal resolution of
$\mathrm{C^{18}O}$(2-1), $\theta=30.2^{\prime\prime}$. Spectral resolution
were set to $0.5\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$
for IRAM-30m data, and $0.25\leavevmode\nobreak\
\mathrm{km\leavevmode\nobreak\ s^{-1}}$ for APEX data. On both panels, the
$\varv_{\mathrm{LSR}}$ of IC443 is indicated with a vertical dashed line (at
$-4.5\leavevmode\nobreak\ \mathrm{km\leavevmode\nobreak\ s^{-1}}$). The black
data points with error bars represent the measurements of the optical depth
$\tau$ corresponding to each channel of these spectra resampled with a
spectral resolution of 2 km s-1, using the [12CO]/[13CO] ratio as a tracer,
and red data points represent the measurements of the optical depth obtained
using the [12CO]/[C18O] ratio. The adopted values for the isotopic ratios are
based on the results of section 4.2.1 and indicated in Tab. 6.

##  Appendix G WISE and 2MASS based classification of infrared point sources
in the extended G region

Table 10: Infrared photometric magnitudes of YSO candidates detected by WISE in the extended G region. ID | Catalog name | W1(3.4 $\upmu$m) | W2(4.6 $\upmu$m) | W3(12 $\upmu$m) | W4(22 $\upmu$m) | Fig. 13 label | $\alpha$ | FLAG
---|---|---|---|---|---|---|---|---
|  | (mag) | (mag) | (mag) | (mag) |  |  |
1 | J061654.93+223403.6 | 17.132 $\pm$ 0.205 | 16.04 $\pm$ 0.25 | 11.906 $\pm$ 0.458 | 8.09 | Class I | 0.99 | 0
2 | J061655.34+223353.3 | 16.925 $\pm$ 0.206 | 15.716 $\pm$ 0.225 | 11.828 $\pm$ 0.52 | 8.654 $\pm$ 0.508 | Class I | 0.86 | 0
3 | J061653.26+223453.7 | 15.348 $\pm$ 0.053 | 13.717 $\pm$ 0.042 | 10.316 $\pm$ 0.085 | 8.234 | Class I | 0.71 | 0
4 | J061656.75+223829.3 | 15.752 $\pm$ 0.068 | 14.049 $\pm$ 0.05 | 10.926 $\pm$ 0.142 | 8.257 | Class I | 0.53 | 0
5 | J061617.53+223155.6 | 12.36 $\pm$ 0.025 | 11.021 $\pm$ 0.021 | 8.844 $\pm$ 0.03 | 5.952 $\pm$ 0.049 | Class I | -0.41 | 0
6 | J061656.48+223943.2 | 11.276 $\pm$ 0.029 | 10.733 $\pm$ 0.027 | 8.612 $\pm$ 0.036 | 6.027 $\pm$ 0.090 | Class II | -0.9 | 0
7 | J061642.63+223825.6 | 15.152 $\pm$ 0.048 | 14.492 $\pm$ 0.066 | 12.316 $\pm$ 0.489 | 8.392 $\pm$ 0.431 | Class II | -0.79 | 0
8 | J061617.19+223356.0 | 14.033 $\pm$ 0.031 | 13.089 $\pm$ 0.032 | 10.99 $\pm$ 0.197 | 7.944 $\pm$ 0.219 | Class II | -0.69 | 0
9 | J061654.18+223456.6 | 14.42 $\pm$ 0.034 | 13.622 $\pm$ 0.038 | 10.85 $\pm$ 0.132 | 8.582 $\pm$ 0.398 | Class II | -0.24 | 0
10 | J061653.02+223444.5 | 15.494 $\pm$ 0.056 | 14.695 $\pm$ 0.077 | 11.238 $\pm$ 0.244 | 8.687 | Class I | 0.29 | 0
11 | J061639.55+223449.3 | 13.393 $\pm$ 0.042 | 12.444 $\pm$ 0.029 | 9.577 $\pm$ 0.371 | 6.398 $\pm$ 0.141 | Class II | -0.09 | 0
12 | J061642.43+223811.8 | 15.687 $\pm$ 0.077 | 14.321 $\pm$ 0.062 | 11.897 $\pm$ 0.407 | 8.415 $\pm$ 0.377 | Class I | -0.2 | 0
13 | J061654.60+223442.0 | 15.628 $\pm$ 0.056 | 14.91 $\pm$ 0.094 | 11.505 $\pm$ 0.258 | 8.369 $\pm$ 0.310 | Class II | 0.21 | 0
14 | J061654.84+223500.4 | 15.476 $\pm$ 0.054 | 14.818 $\pm$ 0.08 | 11.6 $\pm$ 0.299 | 8.268 | Class II | 0.03 | 0
15 | J061640.86+223753.0 | 15.845 $\pm$ 0.069 | 14.826 $\pm$ 0.082 | 11.77 $\pm$ 0.382 | 8.51 $\pm$ 0.493 | Class I | 0.1 | 0
16 | J061638.20+223322.9 | 14.555 $\pm$ 0.049 | 12.846 $\pm$ 0.035 | 9.626 $\pm$ 0.113 | 7.84 $\pm$ 0.366 | Class I | 0.61 | 1
17 | J061638.34+223313.0 | 14.453 $\pm$ 0.059 | 13.053 $\pm$ 0.035 | 9.533 $\pm$ 0.249 | 7.877 $\pm$ 0.323 | Class I | 0.68 | 1
18 | J061643.64+223232.1 | 11.158 $\pm$ 0.028 | 9.394 $\pm$ 0.021 | 6.363 $\pm$ 0.015 | 6.11 $\pm$ 0.145 | Class I | 0.49 | 3
19 | J061646.10+223246.9 | 13.34 $\pm$ 0.028 | 11.706 $\pm$ 0.023 | 8.424 $\pm$ 0.029 | 8.667 | Class I | 0.62 | 3
20 | J061641.30+223044.8 | 15.073 $\pm$ 0.053 | 13.683 $\pm$ 0.044 | 9.385 $\pm$ 0.087 | 8.617 | Class I | 1.28 | 3
21 | J061642.50+223142.4 | 11.168 $\pm$ 0.025 | 9.246 $\pm$ 0.021 | 6.51 $\pm$ 0.015 | 6.217 $\pm$ 0.090 | Class I | 0.35 | 3
22 | J061634.95+223128.1 | 12.786 $\pm$ 0.036 | 10.981 $\pm$ 0.024 | 7.86 $\pm$ 0.027 | 6.443 $\pm$ 0.071 | Class I | 0.59 | 3
23 | J061639.57+223219.9 | 13.203 $\pm$ 0.045 | 11.801 $\pm$ 0.037 | 8.653 $\pm$ 0.13 | 8.272 | Class I | 0.39 | 5
24 | J061632.40+223012.2 | 14.098 $\pm$ 0.036 | 12.352 $\pm$ 0.028 | 8.965 $\pm$ 0.037 | 7.88 $\pm$ 0.305 | Class I | 0.76 | 1
25 | J061642.44+223206.3 | 11.228 $\pm$ 0.028 | 9.299 $\pm$ 0.023 | 6.521 $\pm$ 0.018 | 6.171 $\pm$ 0.103 | Class I | 0.39 | 5
26 | J061643.86+223340.7 | 12.358 $\pm$ 0.048 | 10.323 $\pm$ 0.027 | 7.473 $\pm$ 0.053 | 6.553 | Class I | 0.5 | 3
27 | J061642.75+223108.9 | 13.4 $\pm$ 0.026 | 12.176 $\pm$ 0.026 | 8.98 $\pm$ 0.035 | 7.724 $\pm$ 0.211 | Class I | 0.32 | 3
28 | J061641.63+223111.0 | 12.829 $\pm$ 0.027 | 11.003 $\pm$ 0.023 | 8.096 $\pm$ 0.029 | 7.607 $\pm$ 0.289 | Class I | 0.43 | 5
29 | J061635.24+223521.1 | 14.723 $\pm$ 0.057 | 13.606 $\pm$ 0.042 | 9.478 $\pm$ 0.202 | 7.199 $\pm$ 0.156 | Class I | 1.0 | 1
30 | J061639.81+223201.5 | 12.88 $\pm$ 0.031 | 10.896 $\pm$ 0.023 | 8.251 $\pm$ 0.083 | 8.371 | Class I | 0.31 | 3
31 | J061633.23+223103.7 | 12.862 $\pm$ 0.027 | 11.146 $\pm$ 0.023 | 8.242 $\pm$ 0.043 | 6.932 $\pm$ 0.098 | Class I | 0.37 | 3
32 | J061635.54+223108.5 | 13.757 $\pm$ 0.03 | 12.12 $\pm$ 0.026 | 8.638 $\pm$ 0.039 | 7.456 $\pm$ 0.162 | Class I | 0.78 | 3
33 | J061642.91+223215.9 | 11.159 $\pm$ 0.024 | 9.3 $\pm$ 0.02 | 6.33 $\pm$ 0.014 | 5.976 $\pm$ 0.084 | Class I | 0.5 | 3
34 | J061639.38+223234.8 | 14.358 $\pm$ 0.046 | 13.055 $\pm$ 0.038 | 9.669 $\pm$ 0.23 | 7.606 | Class I | 0.52 | 3
35 | J061640.86+223310.8 | 11.727 $\pm$ 0.023 | 10.662 $\pm$ 0.02 | 8.315 $\pm$ 0.036 | 7.473 $\pm$ 0.244 | Class II | -0.43 | 5
36 | J061647.39+223406.4 | 13.909 $\pm$ 0.03 | 13.397 $\pm$ 0.033 | 10.958 $\pm$ 0.212 | 7.292 | Class II | -0.66 | 3
37 | J061642.00+223339.7 | 10.74 $\pm$ 0.024 | 10.143 $\pm$ 0.02 | 8.244 $\pm$ 0.085 | 6.939 $\pm$ 0.193 | Class II | -1.04 | 3
38 | J061645.55+223335.1 | 12.046 $\pm$ 0.025 | 10.487 $\pm$ 0.021 | 8.433 $\pm$ 0.032 | 7.121 | Class I | -0.39 | 5
39 | J061635.51+223239.1 | 14.932 $\pm$ 0.044 | 13.438 $\pm$ 0.035 | 11.349 $\pm$ 0.366 | 8.485 | Class I | -0.4 | 3
40 | J061644.88+223352.6 | 12.305 $\pm$ 0.039 | 10.132 $\pm$ 0.02 | 7.963 $\pm$ 0.031 | 7.454 $\pm$ 0.442 | Class I | 0.04 | 3
41 | J061642.28+223241.6 | 11.956 $\pm$ 0.034 | 10.024 $\pm$ 0.023 | 7.769 $\pm$ 0.105 | 6.777 $\pm$ 0.128 | Class I | -0.02 | 3
42 | J061643.22+223302.2 | 11.709 $\pm$ 0.027 | 9.96 $\pm$ 0.021 | 7.198 $\pm$ 0.018 | 6.666 $\pm$ 0.254 | Class I | 0.27 | 3
43 | J061647.94+223431.0 | 13.987 $\pm$ 0.032 | 12.795 $\pm$ 0.028 | 9.7 $\pm$ 0.078 | 7.89 | Class I | 0.23 | 3
44 | J061640.55+223121.5 | 12.291 $\pm$ 0.025 | 10.557 $\pm$ 0.023 | 7.939 $\pm$ 0.026 | 7.795 $\pm$ 0.259 | Class I | 0.15 | 5
45 | J061630.48+223009.3 | 14.817 $\pm$ 0.041 | 13.375 $\pm$ 0.042 | 10.875 $\pm$ 0.17 | 8.639 | Class I | -0.1 | 1
46 | J061643.19+223038.8 | 15.019 $\pm$ 0.043 | 13.721 $\pm$ 0.04 | 11.043 $\pm$ 0.184 | 8.752 | Class I | -0.04 | 1
47 | J061650.62+223515.5 | 13.783 $\pm$ 0.032 | 11.77 $\pm$ 0.024 | 9.615 $\pm$ 0.062 | 8.559 $\pm$ 0.490 | Class I | -0.06 | 1
48 | J061641.59+223132.8 | 11.874 $\pm$ 0.029 | 10.064 $\pm$ 0.023 | 7.515 $\pm$ 0.022 | 6.815 $\pm$ 0.146 | Class I | 0.14 | 3
49 | J061640.18+223149.4 | 12.626 $\pm$ 0.031 | 10.845 $\pm$ 0.029 | 8.508 $\pm$ 0.088 | 7.898 | Class I | -0.04 | 5
50 | J061639.32+223320.1 | 14.693 $\pm$ 0.061 | 12.991 $\pm$ 0.035 | 10.655 $\pm$ 0.284 | 7.322 $\pm$ 0.192 | Class I | -0.09 | 1
51 | J061636.38+223308.9 | 13.925 $\pm$ 0.038 | 12.355 $\pm$ 0.027 | 10.027 $\pm$ 0.396 | 7.67 | Class I | -0.17 | 1
52 | J061642.01+223418.9 | 14.356 $\pm$ 0.057 | 12.241 $\pm$ 0.026 | 9.799 $\pm$ 0.462 | 7.823 $\pm$ 0.482 | Class I | 0.23 | 3
53 | J061639.74+223041.6 | 14.382 $\pm$ 0.036 | 12.701 $\pm$ 0.034 | 9.991 $\pm$ 0.347 | 8.641 | Class I | 0.2 | 1
54 | J061646.36+223424.7 | 12.69 $\pm$ 0.027 | 11.661 $\pm$ 0.024 | 8.949 $\pm$ 0.045 | 7.379 $\pm$ 0.251 | Class II | -0.16 | 3
55 | J061645.01+223259.5 | 11.93 $\pm$ 0.024 | 10.383 $\pm$ 0.02 | 7.495 $\pm$ 0.019 | 7.311 $\pm$ 0.138 | Class I | 0.26 | 3
56 | J061643.87+223250.1 | 11.07 $\pm$ 0.024 | 9.276 $\pm$ 0.02 | 6.732 $\pm$ 0.016 | 6.358 $\pm$ 0.194 | Class I | 0.13 | 5
57 | J061635.06+223135.9 | 12.134 $\pm$ 0.026 | 10.475 $\pm$ 0.023 | 7.958 $\pm$ 0.025 | 6.41 $\pm$ 0.073 | Class I | 0.03 | 3
58 | J061647.01+223500.8 | 14.047 $\pm$ 0.035 | 11.907 $\pm$ 0.024 | 9.892 $\pm$ 0.103 | 7.989 | Class I | -0.1 | 3
59 | J061644.84+223442.6 | 12.885 $\pm$ 0.029 | 11.157 $\pm$ 0.026 | 8.788 $\pm$ 0.035 | 7.539 $\pm$ 0.240 | Class I | -0.05 | 3
60 | J061641.36+223012.4 | 13.6 $\pm$ 0.037 | 11.791 $\pm$ 0.027 | 9.673 $\pm$ 0.122 | 7.951 | Class I | -0.2 | 3
61 | J061643.18+223129.7 | 12.525 $\pm$ 0.022 | 11.347 $\pm$ 0.023 | 8.34 $\pm$ 0.024 | 6.933 $\pm$ 0.111 | Class I | 0.15 | 3
62 | J061650.94+223454.3 | 14.969 $\pm$ 0.049 | 12.959 $\pm$ 0.032 | 10.635 $\pm$ 0.144 | 8.476 | Class I | 0.07 | 1
63 | J061644.45+223331.1 | 12.396 $\pm$ 0.035 | 10.456 $\pm$ 0.022 | 7.952 $\pm$ 0.027 | 7.341 | Class I | 0.18 | 3
64 | J061633.49+223110.4 | 12.208 $\pm$ 0.024 | 11.279 $\pm$ 0.027 | 8.486 $\pm$ 0.039 | 7.219 $\pm$ 0.144 | Class II | -0.16 | 3
65 | J061642.76+223402.6 | 12.266 $\pm$ 0.028 | 10.421 $\pm$ 0.021 | 7.897 $\pm$ 0.071 | 7.022 $\pm$ 0.162 | Class I | 0.14 | 3
Table 11: Infrared photometric magnitudes of YSO candidates detected by 2MASS in the extended G region. ID | r.a. | dec. | J(1.25 $\upmu$m) | H(1.65 $\upmu$m) | K(2.17 $\upmu$m) | Fig. 13 label | FLAG
---|---|---|---|---|---|---|---
| (J2000) | (J2000) | (mag) | (mag) | (mag) |  |
1 | $6^{\mathrm{h}}16^{\mathrm{m}}21.16^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}25.37^{\mathrm{s}}$ | 16.073 $\pm$ 0.078 | 15.449 $\pm$ 0.108 | 14.932 $\pm$ 0.093 | YSO | 0
2 | $6^{\mathrm{h}}16^{\mathrm{m}}21.35^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}32.27^{\mathrm{s}}$ | 15.3 $\pm$ 0.048 | 14.92 $\pm$ 0.087 | 14.708 $\pm$ 0.075 | YSO | 0
3 | $6^{\mathrm{h}}16^{\mathrm{m}}32.01^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}59.85^{\mathrm{s}}$ | 16.83 $\pm$ 0.140 | 15.981 $\pm$ 0.182 | 15.234 $\pm$ 0.120 | YSO | 0
4 | $6^{\mathrm{h}}16^{\mathrm{m}}23.77^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}59.89^{\mathrm{s}}$ | 15.138 $\pm$ 0.055 | 14.519 $\pm$ 0.064 | 14.094 $\pm$ 0.046 | YSO | 0
5 | $6^{\mathrm{h}}16^{\mathrm{m}}19.73^{\mathrm{s}}$ | $22^{\mathrm{d}}36^{\mathrm{m}}17.92^{\mathrm{s}}$ | 15.439 $\pm$ 0.074 | 14.997 $\pm$ 0.094 | 14.576 $\pm$ 0.070 | YSO | 0
6 | $6^{\mathrm{h}}16^{\mathrm{m}}21.42^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}33.23^{\mathrm{s}}$ | 15.4 $\pm$ 0.052 | 14.815 $\pm$ 0.069 | 14.347 $\pm$ 0.067 | YSO | 0
7 | $6^{\mathrm{h}}16^{\mathrm{m}}20.25^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}39.30^{\mathrm{s}}$ | 16.75 $\pm$ 0.150 | 16.051 $\pm$ 0.192 | 15.478 $\pm$ 0.136 | YSO | 0
8 | $6^{\mathrm{h}}16^{\mathrm{m}}54.05^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}37.07^{\mathrm{s}}$ | 16.742 $\pm$ 0.165 | 16.013 $\pm$ 0.188 | 15.451 $\pm$ 0.145 | YSO | 0
9 | $6^{\mathrm{h}}16^{\mathrm{m}}39.00^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}00.26^{\mathrm{s}}$ | 16.22 $\pm$ 0.109 | 15.587 $\pm$ 0.144 | 15.226 $\pm$ 0.123 | YSO | 0
10 | $6^{\mathrm{h}}16^{\mathrm{m}}41.73^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}21.36^{\mathrm{s}}$ | 15.163 $\pm$ 0.049 | 14.663 $\pm$ 0.067 | 14.226 $\pm$ 0.054 | YSO | 0
11 | $6^{\mathrm{h}}16^{\mathrm{m}}45.23^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}03.71^{\mathrm{s}}$ | 16.753 $\pm$ 0.170 | 16.174 $\pm$ 0.222 | 15.604 $\pm$ 0.168 | YSO | 0
12 | $6^{\mathrm{h}}16^{\mathrm{m}}37.41^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}45.04^{\mathrm{s}}$ | 16.45 $\pm$ 0.120 | 16.011 $\pm$ 0.188 | 15.756 $\pm$ 0.189 | YSO | 0
13 | $6^{\mathrm{h}}16^{\mathrm{m}}28.65^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}29.60^{\mathrm{s}}$ | 15.273 $\pm$ 0.061 | 14.65 $\pm$ 0.090 | 14.086 $\pm$ 0.059 | YSO | 0
14 | $6^{\mathrm{h}}16^{\mathrm{m}}25.18^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}48.32^{\mathrm{s}}$ | 13.487 $\pm$ 0.027 | 13.011 $\pm$ 0.038 | 12.658 $\pm$ 0.025 | YSO | 0
15 | $6^{\mathrm{h}}16^{\mathrm{m}}25.96^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}57.38^{\mathrm{s}}$ | 15.913 $\pm$ 0.072 | 15.315 $\pm$ 0.105 | 14.878 $\pm$ 0.107 | YSO | 0
16 | $6^{\mathrm{h}}16^{\mathrm{m}}26.89^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}46.11^{\mathrm{s}}$ | 15.278 $\pm$ 0.044 | 14.761 $\pm$ 0.075 | 14.47 $\pm$ 0.068 | YSO | 0
17 | $6^{\mathrm{h}}16^{\mathrm{m}}37.10^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}17.74^{\mathrm{s}}$ | 16.608 $\pm$ 0.148 | 15.972 $\pm$ 0.194 | 15.335 $\pm$ 0.134 | YSO | 0
18 | $6^{\mathrm{h}}16^{\mathrm{m}}18.27^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}49.88^{\mathrm{s}}$ | 14.252 $\pm$ 0.034 | 13.7 $\pm$ 0.034 | 13.392 $\pm$ 0.030 | YSO | 0
19 | $6^{\mathrm{h}}16^{\mathrm{m}}17.72^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}57.65^{\mathrm{s}}$ | 16.62 $\pm$ 0.132 | 16.029 $\pm$ 0.190 | 15.464 $\pm$ 0.145 | YSO | 0
20 | $6^{\mathrm{h}}16^{\mathrm{m}}27.76^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}04.81^{\mathrm{s}}$ | 16.348 $\pm$ 0.106 | 15.627 $\pm$ 0.162 | 15.161 $\pm$ 0.121 | YSO | 0
21 | $6^{\mathrm{h}}16^{\mathrm{m}}39.20^{\mathrm{s}}$ | $22^{\mathrm{d}}36^{\mathrm{m}}57.77^{\mathrm{s}}$ | 17.06 $\pm$ 0.183 | 16.282 $\pm$ 0.235 | 15.662 $\pm$ 0.170 | YSO | 0
22 | $6^{\mathrm{h}}16^{\mathrm{m}}38.84^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}50.51^{\mathrm{s}}$ | 13.85 $\pm$ 0.027 | 13.508 $\pm$ 0.039 | 13.307 $\pm$ 0.031 | YSO | 0
23 | $6^{\mathrm{h}}16^{\mathrm{m}}34.85^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}45.31^{\mathrm{s}}$ | 13.714 $\pm$ 0.031 | 13.268 $\pm$ 0.038 | 12.954 $\pm$ 0.027 | YSO | 0
24 | $6^{\mathrm{h}}16^{\mathrm{m}}32.52^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}19.35^{\mathrm{s}}$ | 14.745 $\pm$ 0.036 | 14.165 $\pm$ 0.055 | 13.813 $\pm$ 0.039 | YSO | 0
25 | $6^{\mathrm{h}}16^{\mathrm{m}}30.79^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}27.47^{\mathrm{s}}$ | 14.896 $\pm$ 0.036 | 14.202 $\pm$ 0.034 | 13.762 $\pm$ 0.039 | YSO | 0
26 | $6^{\mathrm{h}}16^{\mathrm{m}}30.19^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}29.64^{\mathrm{s}}$ | 15.996 $\pm$ 0.079 | 15.408 $\pm$ 0.114 | 14.843 $\pm$ 0.087 | YSO | 0
27 | $6^{\mathrm{h}}16^{\mathrm{m}}33.70^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}27.99^{\mathrm{s}}$ | 14.368 $\pm$ 0.032 | 13.821 $\pm$ 0.047 | 13.487 $\pm$ 0.031 | YSO | 0
28 | $6^{\mathrm{h}}16^{\mathrm{m}}33.83^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}06.52^{\mathrm{s}}$ | 15.865 $\pm$ 0.072 | 15.212 $\pm$ 0.087 | 14.83 $\pm$ 0.078 | YSO | 0
29 | $6^{\mathrm{h}}16^{\mathrm{m}}56.77^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}15.22^{\mathrm{s}}$ | 15.112 $\pm$ 0.042 | 14.755 $\pm$ 0.070 | 14.461 $\pm$ 0.060 | YSO | 0
30 | $6^{\mathrm{h}}16^{\mathrm{m}}53.13^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}03.76^{\mathrm{s}}$ | 15.879 $\pm$ 0.082 | 15.605 $\pm$ 0.149 | 15.273 $\pm$ 0.131 | YSO | 0
31 | $6^{\mathrm{h}}16^{\mathrm{m}}57.99^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}04.98^{\mathrm{s}}$ | 14.739 $\pm$ 0.037 | 14.366 $\pm$ 0.057 | 14.057 $\pm$ 0.048 | YSO | 0
32 | $6^{\mathrm{h}}16^{\mathrm{m}}48.47^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}57.35^{\mathrm{s}}$ | 11.835 $\pm$ 0.023 | 11.741 $\pm$ 0.030 | 11.69 $\pm$ 0.023 | YSO | 0
33 | $6^{\mathrm{h}}16^{\mathrm{m}}49.15^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}37.91^{\mathrm{s}}$ | 16.26 $\pm$ 0.100 | 15.794 $\pm$ 0.152 | 15.355 $\pm$ 0.129 | YSO | 0
34 | $6^{\mathrm{h}}16^{\mathrm{m}}51.04^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}16.69^{\mathrm{s}}$ | 16.806 $\pm$ 0.178 | 16.093 $\pm$ 0.223 | 15.637 $\pm$ 0.169 | YSO | 0
35 | $6^{\mathrm{h}}16^{\mathrm{m}}52.65^{\mathrm{s}}$ | $22^{\mathrm{d}}32^{\mathrm{m}}10.02^{\mathrm{s}}$ | 15.536 $\pm$ 0.056 | 14.916 $\pm$ 0.077 | 14.473 $\pm$ 0.063 | YSO | 0
36 | $6^{\mathrm{h}}16^{\mathrm{m}}56.50^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}43.29^{\mathrm{s}}$ | 14.008 $\pm$ 0.038 | 13.187 $\pm$ 0.041 | 12.502 $\pm$ 0.028 | YSO | 0
37 | $6^{\mathrm{h}}16^{\mathrm{m}}49.04^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}47.80^{\mathrm{s}}$ | 14.418 $\pm$ 0.033 | 14.196 $\pm$ 0.048 | 13.853 $\pm$ 0.044 | YSO | 0
38 | $6^{\mathrm{h}}16^{\mathrm{m}}49.76^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}12.79^{\mathrm{s}}$ | 15.869 $\pm$ 0.078 | 15.481 $\pm$ 0.123 | 15.182 $\pm$ 0.117 | YSO | 0
39 | $6^{\mathrm{h}}16^{\mathrm{m}}58.80^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}58.44^{\mathrm{s}}$ | 11.262 $\pm$ 0.022 | 10.979 $\pm$ 0.030 | 10.796 $\pm$ 0.021 | YSO | 0
40 | $6^{\mathrm{h}}16^{\mathrm{m}}52.79^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}39.43^{\mathrm{s}}$ | 16.178 $\pm$ 0.103 | 16.14 $\pm$ 0.228 | 15.496 $\pm$ 0.164 | YSO | 0
41 | $6^{\mathrm{h}}16^{\mathrm{m}}51.69^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}37.42^{\mathrm{s}}$ | 15.277 $\pm$ 0.052 | 14.827 $\pm$ 0.074 | 14.372 $\pm$ 0.081 | YSO | 0
42 | $6^{\mathrm{h}}16^{\mathrm{m}}40.28^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}17.54^{\mathrm{s}}$ | 15.355 $\pm$ 0.056 | 14.797 $\pm$ 0.082 | 14.487 $\pm$ 0.068 | YSO | 0
43 | $6^{\mathrm{h}}16^{\mathrm{m}}41.82^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}30.09^{\mathrm{s}}$ | 16.673 $\pm$ 0.158 | 16.052 $\pm$ 0.215 | 15.654 $\pm$ 0.167 | YSO | 0
44 | $6^{\mathrm{h}}16^{\mathrm{m}}44.95^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}49.96^{\mathrm{s}}$ | 15.919 $\pm$ 0.081 | 15.28 $\pm$ 0.100 | 14.832 $\pm$ 0.086 | YSO | 0
45 | $6^{\mathrm{h}}16^{\mathrm{m}}50.66^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}20.93^{\mathrm{s}}$ | 14.637 $\pm$ 0.040 | 14.328 $\pm$ 0.057 | 14.092 $\pm$ 0.055 | YSO | 0
46 | $6^{\mathrm{h}}16^{\mathrm{m}}18.14^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}18.74^{\mathrm{s}}$ | 16.236 $\pm$ 0.102 | 15.326 $\pm$ 0.118 | 14.713 $\pm$ 0.069 | CTTS | 0
47 | $6^{\mathrm{h}}16^{\mathrm{m}}20.71^{\mathrm{s}}$ | $22^{\mathrm{d}}36^{\mathrm{m}}44.49^{\mathrm{s}}$ | 16.83 $\pm$ 0.163 | 16.054 $\pm$ 0.190 | 15.544 $\pm$ 0.151 | CTTS | 0
48 | $6^{\mathrm{h}}16^{\mathrm{m}}31.07^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}20.79^{\mathrm{s}}$ | 17.069 $\pm$ 0.203 | 15.948 $\pm$ 0.175 | 15.21 $\pm$ 0.128 | CTTS | 0
49 | $6^{\mathrm{h}}16^{\mathrm{m}}28.25^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}54.94^{\mathrm{s}}$ | 15.992 $\pm$ 0.094 | 15.117 $\pm$ 0.090 | 14.573 $\pm$ 0.072 | CTTS | 0
50 | $6^{\mathrm{h}}16^{\mathrm{m}}32.20^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}52.98^{\mathrm{s}}$ | 17.311 $\pm$ 0.228 | 15.919 $\pm$ 0.169 | 15.075 $\pm$ 0.112 | CTTS | 0
51 | $6^{\mathrm{h}}16^{\mathrm{m}}25.32^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}29.40^{\mathrm{s}}$ | 16.402 $\pm$ 0.098 | 15.57 $\pm$ 0.136 | 14.91 $\pm$ 0.093 | CTTS | 0
52 | $6^{\mathrm{h}}16^{\mathrm{m}}41.39^{\mathrm{s}}$ | $22^{\mathrm{d}}32^{\mathrm{m}}57.89^{\mathrm{s}}$ | 16.827 $\pm$ 0.180 | 15.657 $\pm$ 0.153 | 14.944 $\pm$ 0.111 | CTTS | 0
53 | $6^{\mathrm{h}}16^{\mathrm{m}}28.97^{\mathrm{s}}$ | $22^{\mathrm{d}}32^{\mathrm{m}}39.40^{\mathrm{s}}$ | 15.688 $\pm$ 0.056 | 14.903 $\pm$ 0.064 | 14.459 $\pm$ 0.064 | CTTS | 0
54 | $6^{\mathrm{h}}16^{\mathrm{m}}25.67^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}06.09^{\mathrm{s}}$ | 17.201 $\pm$ 0.219 | 16.343 $\pm$ 0.262 | 15.773 $\pm$ 0.198 | CTTS | 0
55 | $6^{\mathrm{h}}16^{\mathrm{m}}34.49^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}22.21^{\mathrm{s}}$ | 16.21 $\pm$ 0.084 | 15.149 $\pm$ 0.084 | 14.537 $\pm$ 0.063 | CTTS | 0
56 | $6^{\mathrm{h}}16^{\mathrm{m}}30.92^{\mathrm{s}}$ | $22^{\mathrm{d}}36^{\mathrm{m}}01.72^{\mathrm{s}}$ | 16.564 $\pm$ 0.128 | 15.298 $\pm$ 0.110 | 14.436 $\pm$ 0.062 | CTTS | 0
57 | $6^{\mathrm{h}}16^{\mathrm{m}}30.75^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}28.69^{\mathrm{s}}$ | 16.132 $\pm$ 0.079 | 15.328 $\pm$ 0.099 | 14.737 $\pm$ 0.077 | CTTS | 0
58 | $6^{\mathrm{h}}16^{\mathrm{m}}32.27^{\mathrm{s}}$ | $22^{\mathrm{d}}39^{\mathrm{m}}32.10^{\mathrm{s}}$ | 16.987 $\pm$ 0.166 | 15.842 $\pm$ 0.152 | 15.084 $\pm$ 0.107 | CTTS | 0
59 | $6^{\mathrm{h}}16^{\mathrm{m}}50.15^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}04.16^{\mathrm{s}}$ | 16.416 $\pm$ 0.122 | 15.609 $\pm$ 0.138 | 15.122 $\pm$ 0.105 | CTTS | 0
60 | $6^{\mathrm{h}}16^{\mathrm{m}}49.96^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}43.88^{\mathrm{s}}$ | 16.521 $\pm$ 0.136 | 15.645 $\pm$ 0.143 | 15.08 $\pm$ 0.113 | CTTS | 0
61 | $6^{\mathrm{h}}16^{\mathrm{m}}54.18^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}56.75^{\mathrm{s}}$ | 16.184 $\pm$ 0.098 | 15.279 $\pm$ 0.107 | 14.72 $\pm$ 0.076 | CTTS | 0
62 | $6^{\mathrm{h}}16^{\mathrm{m}}48.71^{\mathrm{s}}$ | $22^{\mathrm{d}}36^{\mathrm{m}}02.72^{\mathrm{s}}$ | 16.682 $\pm$ 0.152 | 15.854 $\pm$ 0.171 | 15.249 $\pm$ 0.126 | CTTS | 0
63 | $6^{\mathrm{h}}16^{\mathrm{m}}20.50^{\mathrm{s}}$ | $22^{\mathrm{d}}37^{\mathrm{m}}06.78^{\mathrm{s}}$ | 15.847 $\pm$ 0.074 | 15.298 $\pm$ 0.102 | 14.635 $\pm$ 0.083 | HAeBe | 0
64 | $6^{\mathrm{h}}16^{\mathrm{m}}20.35^{\mathrm{s}}$ | $22^{\mathrm{d}}35^{\mathrm{m}}04.23^{\mathrm{s}}$ | 15.896 $\pm$ 0.073 | 15.477 $\pm$ 0.110 | 14.917 $\pm$ 0.100 | HAeBe | 0
65 | $6^{\mathrm{h}}16^{\mathrm{m}}37.47^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}53.17^{\mathrm{s}}$ | 16.922 $\pm$ 0.187 | 16.207 $\pm$ 0.243 | 15.484 $\pm$ 0.150 | HAeBe | 0
66 | $6^{\mathrm{h}}16^{\mathrm{m}}25.69^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}08.44^{\mathrm{s}}$ | 16.448 $\pm$ 0.140 | 15.86 $\pm$ 0.161 | 15.218 $\pm$ 0.132 | HAeBe | 0
67 | $6^{\mathrm{h}}16^{\mathrm{m}}31.69^{\mathrm{s}}$ | $22^{\mathrm{d}}38^{\mathrm{m}}17.72^{\mathrm{s}}$ | 16.433 $\pm$ 0.108 | 16.133 $\pm$ 0.215 | 15.392 $\pm$ 0.138 | HAeBe | 0
68 | $6^{\mathrm{h}}16^{\mathrm{m}}57.74^{\mathrm{s}}$ | $22^{\mathrm{d}}30^{\mathrm{m}}24.12^{\mathrm{s}}$ | 16.068 $\pm$ 0.092 | 15.669 $\pm$ 0.144 | 15.076 $\pm$ 0.101 | HAeBe | 0
69 | $6^{\mathrm{h}}16^{\mathrm{m}}57.50^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}34.24^{\mathrm{s}}$ | 16.757 $\pm$ 0.159 | 16.112 $\pm$ 0.217 | 15.46 $\pm$ 0.157 | HAeBe | 0
70 | $6^{\mathrm{h}}16^{\mathrm{m}}43.12^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}01.40^{\mathrm{s}}$ | 14.73 $\pm$ 0.042 | 14.126 $\pm$ 0.053 | 13.625 $\pm$ 0.086 | YSO | 2
71 | $6^{\mathrm{h}}16^{\mathrm{m}}35.10^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}33.98^{\mathrm{s}}$ | 15.086 $\pm$ 0.048 | 14.306 $\pm$ 0.051 | 13.628 $\pm$ 0.056 | YSO | 2
72 | $6^{\mathrm{h}}16^{\mathrm{m}}44.82^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}42.82^{\mathrm{s}}$ | 15.207 $\pm$ 0.049 | 14.728 $\pm$ 0.067 | 14.395 $\pm$ 0.061 | YSO | 2
73 | $6^{\mathrm{h}}16^{\mathrm{m}}40.21^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}15.34^{\mathrm{s}}$ | 16.192 $\pm$ 0.104 | 15.358 $\pm$ 0.119 | 14.831 $\pm$ 0.119 | CTTS | 2
74 | $6^{\mathrm{h}}16^{\mathrm{m}}41.46^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}28.03^{\mathrm{s}}$ | 15.451 $\pm$ 0.061 | 14.421 $\pm$ 0.058 | 13.757 $\pm$ 0.061 | CTTS | 2
75 | $6^{\mathrm{h}}16^{\mathrm{m}}43.47^{\mathrm{s}}$ | $22^{\mathrm{d}}31^{\mathrm{m}}55.73^{\mathrm{s}}$ | 16.435 $\pm$ 0.121 | 15.65 $\pm$ 0.139 | 15.131 $\pm$ 0.135 | CTTS | 2
76 | $6^{\mathrm{h}}16^{\mathrm{m}}44.87^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}10.32^{\mathrm{s}}$ | 14.743 $\pm$ 0.046 | 14.039 $\pm$ 0.057 | 13.62 $\pm$ 0.072 | CTTS | 1
77 | $6^{\mathrm{h}}16^{\mathrm{m}}45.52^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}42.53^{\mathrm{s}}$ | 16.511 $\pm$ 0.132 | 15.626 $\pm$ 0.144 | 15.116 $\pm$ 0.162 | CTTS | 2
78 | $6^{\mathrm{h}}16^{\mathrm{m}}45.50^{\mathrm{s}}$ | $22^{\mathrm{d}}34^{\mathrm{m}}58.63^{\mathrm{s}}$ | 16.432 $\pm$ 0.130 | 15.51 $\pm$ 0.140 | 14.975 $\pm$ 0.135 | CTTS | 1
79 | $6^{\mathrm{h}}16^{\mathrm{m}}43.49^{\mathrm{s}}$ | $22^{\mathrm{d}}33^{\mathrm{m}}37.44^{\mathrm{s}}$ | 16.867 $\pm$ 0.189 | 15.85 $\pm$ 0.178 | 14.899 $\pm$ 0.148 | HAeBe | 2