# HCO+ and Radio Continuum Emission from the Star Forming Region G75.78+0.34

Authors: Rogemar A. Riffel; Everton Lüdke
Journal: Advances in Astronomy
 (2014)

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## Abstract

We present 1.3 and 3.6 cm radio continuum images and a HCO+ spectrum of the massive star forming region G75.78+0.34 obtained with the Very Large Array (VLA) and with the Berkley Illinois Maryland Association (BIMA) interferometer. Three structures were detected in the continuum emission: one associated with the well-known cometary H ɪɪ region, plus two more compact structures located at 6′′ east and at 2′′ south of cometary H ɪɪ region. Using the total flux and intensity peak we estimated an electron density of ≈1.5 × 104 cm−3, an emission measure of ≈6 × 107 cm−6 pc, a mass of ionized gas of ≈3 M⊙, and a diameter of 0.05 pc for the cometary H ɪɪ region, being typical values for an ultracompact H ɪɪ region. The HCO+ emission probably originates from the molecular outflows previously observed in HCN and CO.


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## Body

## 1. Introduction

H ɪɪ regions are classified as ultracompact, compact, and classical according to their sizes, ionized gas masses, densities, and emission measures (e.g., [1]). Classical H ɪɪ regions such as the Orion Nebulae have sizes of ~10 pc, densities of ~100 cm3, ~105 M⊙ of ionized gas, and EM ~ 102 pc cm6. Compact H ɪɪ regions have densities ≳5 × 103 cm3, sizes of ≲0.5 pc, ionized gas mass of ~1 M⊙, and EM ≳ 107 pc cm−6 while ultracompact H ɪɪ regions have sizes of ≲0.1 pc, and thermal electron densities of ≳104 cm3, mass of ionized gas of ~10−2 M⊙, and EM ≳ 107 pc cm−6 [2, 3].The study of the physical properties of H ɪɪ regions and their classification is a fundamental key to understand how they evolute and how stars form. The radio continuum emission at centimeter wavelengths traces the emission of the ionized gas. On the other hand, the study of the molecular gas next to H ɪɪ regions provides significant information about these objects and issues of star formation theory applied to these objects. So far, most of the studies of the molecular gas are based on CO emission, which has a low dipole moment, implying that low rotational transitions do not trace dense gas, while molecules with higher dipole moments can be used to observe high density gas. The high density cores (n ~ 104-105 cm3) can be studied from mm and submm line emission of the HCN and HCO+ molecules [4].In this work, we use 1.3 and 3.6 cm Very Large Array images to study the physical conditions of the gas in the ultracompact H ɪɪ region G75.78+0.34, as well as Berkley Illinois Maryland Association (BIMA) interferometric data at 3 mm. This object presents a well-known molecular outflow observed in CO [5, 6] and HCN [7] is located in the giant molecular cloud ON2 and was firstly identified by Matthews et al. [8] with observations at 5 and 10.7 GHz. Sánchez-Monge et al. [9] used the VLA observations to study the gas content of G75.78+0.34. They found radio emission coming from three components: a cometary ultracompact H ɪɪ region, excited by a B0 type star, and with no associated dust emission, an almost unresolved ultracompact H ɪɪ region, associated with a compact dust clump detected at millimetric and midinfrared wavelengths, and a compact source embedded in a dust condensation. The continuum emission at 3.5 mm of G75.78+0.34 is dominated by free-free emission from the ionized gas surrounding the exciting star and dust emission may contribute only to a small fraction of its 3.5 mm continuum [7].This paper is organized as follows. In Section2 we describe the observations. Section 3 presents our results, which are discussed in Section 4. The conclusions of this work are presented in Section 5.


## 2. Observations

### 2.1. The BIMA Data

The observations of the emission of HCO+ (J = 1-0) at 89.1885 GHz and HCN (J = 1-0) at 88.63 GHz from G75.78+0.34 and G75.77+0.34 were performed with the Berkley Illinois Maryland Association (BIMA) interferometer by Welch et al. [10] in June, 1999, using its shortest baseline configuration (D-array).Mars and 3C273 observations were used as primary amplitude and bandpass calibrators and the data reduction followed standard procedures with the software MIRIAD by Sault et al. [11]. The full width at half maximum (FWHM) of the synthesized map is about 18 arcsec and the resulting velocity sampling is δV≈ 0.34 km s−1. The HCN emission has already been presented and discussed in Riffel and Lüdke [7], where more details about the observations and data reduction process can be found. Here, we present and discuss the spectrum for the HCO+.


### 2.2.  Radio Continuum Images

We used Very Large Array (VLA) radiocontinuum observations of G75.78+0.34 at 8.46 GHz (3.6 cm) and 22.46 GHz (1.3 cm) from the VLA data archive (program ID: AK440) obtained using the interferometric array at configuration “A”. These observations were processed following the standard procedure of VLA radio continuum imaging processing using the NRAO Astronomical Image Processing System (AIPS). The angular resolutions at these frequencies are 0′′.24 and 0′′.08 for 3.6 cm and 1.3 cm observations, respectively. These resolutions correspond to a spatial resolution of 6.5 × 10−32009pc and 2.2 × 10−3 pc assuming a distance of 5.6 kpc to G75.78+0.34 [12] from which we estimate that the sizes of the main components A, B, and C are, respectively, 0.065, 0.013, and 0.027 pc.


## 2.1. The BIMA Data

The observations of the emission of HCO+ (J = 1-0) at 89.1885 GHz and HCN (J = 1-0) at 88.63 GHz from G75.78+0.34 and G75.77+0.34 were performed with the Berkley Illinois Maryland Association (BIMA) interferometer by Welch et al. [10] in June, 1999, using its shortest baseline configuration (D-array).Mars and 3C273 observations were used as primary amplitude and bandpass calibrators and the data reduction followed standard procedures with the software MIRIAD by Sault et al. [11]. The full width at half maximum (FWHM) of the synthesized map is about 18 arcsec and the resulting velocity sampling is δV≈ 0.34 km s−1. The HCN emission has already been presented and discussed in Riffel and Lüdke [7], where more details about the observations and data reduction process can be found. Here, we present and discuss the spectrum for the HCO+.


## 2.2.  Radio Continuum Images

We used Very Large Array (VLA) radiocontinuum observations of G75.78+0.34 at 8.46 GHz (3.6 cm) and 22.46 GHz (1.3 cm) from the VLA data archive (program ID: AK440) obtained using the interferometric array at configuration “A”. These observations were processed following the standard procedure of VLA radio continuum imaging processing using the NRAO Astronomical Image Processing System (AIPS). The angular resolutions at these frequencies are 0′′.24 and 0′′.08 for 3.6 cm and 1.3 cm observations, respectively. These resolutions correspond to a spatial resolution of 6.5 × 10−32009pc and 2.2 × 10−3 pc assuming a distance of 5.6 kpc to G75.78+0.34 [12] from which we estimate that the sizes of the main components A, B, and C are, respectively, 0.065, 0.013, and 0.027 pc.


## 3. Results

### 3.1. Continuum Emission

In Figure1 we show the 1.3 cm continuum image of G75.78+34, showing thee components identified as A, B, and C in the figure. Our image is in good agreement with the one presented by Sánchez-Monge et al. [9] using the same instrument configuration. The component A shows a complex structure, being more extended to the north-south direction and presenting at least two knots of higher emission. It is associated with the cometary H ɪɪ region observed at 6 cm by Wood and Churchwell [12] and their image appears to be smoother than ours, probably because of its lower spatial resolution. On the other hand, the components B and C are more compact and were not detected at 6 cm. The component C is cospatial with the water maser emission detected by Hofner and Churchwell [13].Figure 1
1.3 cm radio continuum image of G75.78+0.34 obtained with VLA at “A” configuration. Flux levels are 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0 mJy/beam.The 3.6 cm image of G75.78+0.34 is shown in Figure2, showing the same three components observed at the 1.3 cm image. The complex structure seen for the component A at 1.3 cm is not seen at 3.6 cm image, because of its lower spatial resolution. Our 3.6 cm image is very similar to the one shown by Wood and Churchwell [12]. The linear sizes of the components seen at 3.6 cm image are similar to those listed above for the 1.3 cm image.Figure 2
3.5 cm radio continuum image of G75.78+0.34 obtained with VLA at “A” configuration. Flux levels are 0.36, 0.72, 1.08, 1.44, 1.80, 2.16, 2.52, 2.88, 3.24, and 3.6 mJy/beam.Table1 presents the measured total flux (Sν) and the peak intensity (Iν) for each component identified in Figures 1 and 2 at 1.3 cm and 3.6 cm, respectively.Table 1
Total flux and peak intensity for each component of G75.78+0.34 at 1.3 cm and 3.6 cm.
Component
A
B
C
S
ν (1.3 cm) (mJy)
42.4
8.6
8.2
S
ν (3.6 cm) (mJy)
50.4
4.7
1.6
I
ν (1.3 cm) (mJy/beam)
6.7
8.4
5.9
I
ν (3.6 cm) (mJy/beam)
3.6
3.4
1.0


### 3.2. HCO+ Line Emission

The signal-to-noise ratio of our BIMA observations was not high enough to construct emission line flux maps and channel maps across the HCO+ profile for BIMA in the closest spacing configuration with hybrid self-calibration and closure mapping, as we were able to do for the HCN in Riffel and Lüdke [7] discussed as our first results. The HCO+ spectrum is shown in Figure 3 and it was obtained by integrating over the whole field of our BIMA observations and includes both G75.78+0.34 and G75.77+0.34 H ɪɪ regions. The HCO+ emission shows three intensity peaks, at 89.193, 89.195, and 89.197 GHz, suggesting the presence of HCO+ clouds with distinct kinematics.Figure 3
HCO+ spectrum for G75.78+0.34 and G75.77+0.34 from BIMA observations. The intensities are shown in arbitrary correlator units.


## 3.1. Continuum Emission

In Figure1 we show the 1.3 cm continuum image of G75.78+34, showing thee components identified as A, B, and C in the figure. Our image is in good agreement with the one presented by Sánchez-Monge et al. [9] using the same instrument configuration. The component A shows a complex structure, being more extended to the north-south direction and presenting at least two knots of higher emission. It is associated with the cometary H ɪɪ region observed at 6 cm by Wood and Churchwell [12] and their image appears to be smoother than ours, probably because of its lower spatial resolution. On the other hand, the components B and C are more compact and were not detected at 6 cm. The component C is cospatial with the water maser emission detected by Hofner and Churchwell [13].Figure 1
1.3 cm radio continuum image of G75.78+0.34 obtained with VLA at “A” configuration. Flux levels are 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0 mJy/beam.The 3.6 cm image of G75.78+0.34 is shown in Figure2, showing the same three components observed at the 1.3 cm image. The complex structure seen for the component A at 1.3 cm is not seen at 3.6 cm image, because of its lower spatial resolution. Our 3.6 cm image is very similar to the one shown by Wood and Churchwell [12]. The linear sizes of the components seen at 3.6 cm image are similar to those listed above for the 1.3 cm image.Figure 2
3.5 cm radio continuum image of G75.78+0.34 obtained with VLA at “A” configuration. Flux levels are 0.36, 0.72, 1.08, 1.44, 1.80, 2.16, 2.52, 2.88, 3.24, and 3.6 mJy/beam.Table1 presents the measured total flux (Sν) and the peak intensity (Iν) for each component identified in Figures 1 and 2 at 1.3 cm and 3.6 cm, respectively.Table 1
Total flux and peak intensity for each component of G75.78+0.34 at 1.3 cm and 3.6 cm.
Component
A
B
C
S
ν (1.3 cm) (mJy)
42.4
8.6
8.2
S
ν (3.6 cm) (mJy)
50.4
4.7
1.6
I
ν (1.3 cm) (mJy/beam)
6.7
8.4
5.9
I
ν (3.6 cm) (mJy/beam)
3.6
3.4
1.0


## 3.2. HCO+ Line Emission

The signal-to-noise ratio of our BIMA observations was not high enough to construct emission line flux maps and channel maps across the HCO+ profile for BIMA in the closest spacing configuration with hybrid self-calibration and closure mapping, as we were able to do for the HCN in Riffel and Lüdke [7] discussed as our first results. The HCO+ spectrum is shown in Figure 3 and it was obtained by integrating over the whole field of our BIMA observations and includes both G75.78+0.34 and G75.77+0.34 H ɪɪ regions. The HCO+ emission shows three intensity peaks, at 89.193, 89.195, and 89.197 GHz, suggesting the presence of HCO+ clouds with distinct kinematics.Figure 3
HCO+ spectrum for G75.78+0.34 and G75.77+0.34 from BIMA observations. The intensities are shown in arbitrary correlator units.


## 4. Discussion

### 4.1. Ionized Gas

The radio continuum images presented here can be used to investigate the properties of the ionized gas associated with G75.78+0.34. We can use the total fluxes and peak intensities from Table1 to calculate some physical parameters for the component A associated with the cometary H ɪɪ region. Following Panagia and Walmsley [14] under the assumption that the H ɪɪ region has a roughly spherical geometry, we can obtain the electron density (Ne) by
(1)(Ne/cm-3)=3.113×102(Sν/Jy)0.5(Te/104K)0.25×(D/kpc)-0.5b(ν,T)-0.5θR-1.5,
where Sν is the total flux, Te is the electron temperature, D is the distance to the object, θR is the angular radius in arcminutes, and
(2)b(ν,T)=1+0.3195log⁡⁡(Te/104K)-0.2130log⁡⁡(ν/1GHz).The emission measure is given by the following equation:(3)(EM/cm-6pc)=5.638104(Sν/Jy)(Te/104K)b(ν,T)θR-2.The mass of ionized gas can be obtained by [14]
(4)(M/M⊙)=0.7934(Sν/Jy)0.5(Te/104K)0.25(D/kpc)2.5×b(ν,T)-0.5θR1.5(1+Y)-1,
where Y is the abundance of He+ relative to H+.The brightness temperature for a compact radio source is given by (e.g., [12])
(5)Tb=Iν10-29c22ν2kΩb,
where ν is the frequency, Iν is the peak intensity in mJy/beam, k is the Boltzmann constant, and Ωb is the solid angle of the beam given by (e.g., [15])
(6)Ωb=1.133Θb2,
where Θb is the angular resolution of the observations in radians.Finally, the optical depth (τ) is estimated using
(7)Tb=Te(1-e-τ).In order to obtain the physical parameters above, we assumed typical values for the electron temperature and abundance ofTe=104 K and Y=0.07, respectively. Using the equations above and the angular resolutions of Section 2, we obtain b(ν,Te)=0.7121 and Ωb=1.7×10-13 sr for the 1.3 cm image and b(ν,Te)=0.8025 and  Ωb=1.5×10-12 sr for the 3.6 cm image. The radius (ΘR) of the component A can be measured directly from Figures 1 and 2 and, thus, we can estimate relevant physical parameters for G75.78+0.34.In Table2 we present the physical parameters estimated by the equations above, which can be compared with previous estimates from the literature. The values obtained for the electron density are in reasonable agreement with those obtained by Wood and Churchwell [12] from the 6 cm radio emission (Ne=2.7×104 cm−3) and with the value obtained from 7 mm observations  -Ne≈5×104 cm−3 [16], as well as with the one found by Sánchez-Monge et al. [9] from a multifrequency study (Ne=3.7×104 cm−3). The emission measure found here is between the values found by Matthews et al. [17] of EM=1.1×106 cm−6 pc, by Wood and Churchwell [12] of EM=2.3×106 cm−6 pc, and by Sánchez-Monge et al. [9] of EM=2.5×107 cm−6 pc. Wood and Churchwell [12] found Tb=2300 K and τ=0.27, and thus, our values obtained from the 1.3 cm emission are in good agreement with theirs, while those estimated from the 3.6 cm are a bit smaller. The mass of G75.78+0.34 obtained here is about one order of magnitude smaller than the value found by Matthews et al. [17] and about one order of magnitude larger than the value obtained by Sánchez-Monge et al. [9], probably due to differences in the size of the region used to integrate the flux by these authors and by us, as well as due to the assumptions used in the calculations. The parameters presented in Table 2 confirm that G75.78+0.34 is an ultracompact H ɪɪ region [3], confirming previous results of Sánchez-Monge et al. [9].Table 2
Physical parameters obtained for the cometary HII region G75.78+0.34 from the 1.3 cm and 3.6 cm images.
Parameter
1.3 cm
3.6 cm
θ
R (arc sec)
0.9
1.2
N
e
(
cm
-
3
)
1.7
×
1
0
4
1.2
×
1
0
4
EM (cm-6pc)
7.6
×
1
0
6
5.1
×
1
0
6
M (M⊙)
2.5
×
1
0
-
2
3.9
×
1
0
-
2
T
b (K)
2530
1100
τ
0.29
0.12
Diameter (pc)
0.05
0.06For the components B and C, we estimate the physical parameters using only the 1.3 cm image, since it has the highest spatial resolution. For the component B, we obtainNe≈3.3×105 cm−3, EM≈1.9×107 cm−6 pc, and a mass of ionized gas of M≈1.6×10-3 M⊙, assuming a radius of 0.25 arcsec for the region. Assuming a radius of 0.4 arcsec for the component C, we obtain Ne≈1.6×105 cm−3, EM≈7.4×106 cm−6 pc, and M≈3×10-3 M⊙. These values are similar to those expected for ultracompact H ɪɪ regions [2, 3]. In fact, Sánchez-Monge et al. [9] identified the component C as being an ultracompact H ɪɪ region associated with dust emission in the millimetric and midinfrared wavelengths, while the component B seems to be embedded in dust.


### 4.2.  Molecular Gas

Although the signal-to-noise ratio of the HCO+ data was not high enough to construct flux and channel maps, as it has been done for the HCN in Riffel and Lüdke [7] using the same data, its detection can tell us some information about the star forming region G75.78+0.34. The complex line profile shown in Figure 3 suggests that the HCO+ emission originate from gas with a disturbed kinematics and since it usually originate from high density gas, the HCO+ emission may be tracing also the bipolar molecular outflows observed in HCN for G75.78+0.34 in our previous paper. A similar conclusion has been presented for the Serpens star forming region using BIMA observations by Hogerheijde [18], for which it is found that the HCN and HCO+ present enhanced emission near outflows, while the N2H+ reflects the distribution of the cloud.


#### 4.2.1. SEST Observations and The Nondetection of SiO Emission

Besides the BIMA data, we have also employed the Swedish-ESO Submillimeter Telescope (SEST) in 20th April 2003 in order to detect higher excitation lines like SiO (2-1 at 86.646 GHz), SiO (3-2 at 130.268 GHz), SiO (5-4 at 217.104 GHz), and SiO (8-7, 347.330 GHz) to make a spectral line survey of maser emission from G75.78+0.34 and G75.77+0.34 at higher excitations. Even with longer integration times of about one hour per transition, we were unable to detect these lines at a confidence better than 5σ above the instrumental noise level.On the other hand, the H13CN at 86.338 GHz was present in our SEST observations, presenting a profile similar to the one of the HCN (1-0) suggesting that the emission may occur within zones of similar physical and kinematical conditions. Our observations therefore suggest that SiO lines may not be good observational tracers of shock-driven outflows in G75.78+0.34.This conclusion is supported in a similar result obtained for the star forming core W3-SE using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by Zhu et al. [19], in which the authors report the detection of the HCO+ associated with outflows, while the SiO (2-1) line at 86.243 GHz was also not detected for W3-SE in independent observations. This certainly brings the fact that there are difficulties in using SiO to obtain information on the astrophysical conditions of this compact object within the production of SiO by destruction of dust grains by radiatively driven MHD shock front from young and massive stars.On the other hand, we must emphasize that there are several works for UCH ɪɪ regions and more evolved objects showing that the SiO is a good tracer of outflows (e.g., [20–22]) and a possible explanation for the absence of excited SiO lines in G75.78+0.34 could be due to low sensitivity of the SEST observations. New and more sensitivity observations are henceforth needed to better constrain the SiO emission or its absence in G75.78+0.34 and to unravel such apparently contradictory statements.


## 4.1. Ionized Gas

The radio continuum images presented here can be used to investigate the properties of the ionized gas associated with G75.78+0.34. We can use the total fluxes and peak intensities from Table1 to calculate some physical parameters for the component A associated with the cometary H ɪɪ region. Following Panagia and Walmsley [14] under the assumption that the H ɪɪ region has a roughly spherical geometry, we can obtain the electron density (Ne) by
(1)(Ne/cm-3)=3.113×102(Sν/Jy)0.5(Te/104K)0.25×(D/kpc)-0.5b(ν,T)-0.5θR-1.5,
where Sν is the total flux, Te is the electron temperature, D is the distance to the object, θR is the angular radius in arcminutes, and
(2)b(ν,T)=1+0.3195log⁡⁡(Te/104K)-0.2130log⁡⁡(ν/1GHz).The emission measure is given by the following equation:(3)(EM/cm-6pc)=5.638104(Sν/Jy)(Te/104K)b(ν,T)θR-2.The mass of ionized gas can be obtained by [14]
(4)(M/M⊙)=0.7934(Sν/Jy)0.5(Te/104K)0.25(D/kpc)2.5×b(ν,T)-0.5θR1.5(1+Y)-1,
where Y is the abundance of He+ relative to H+.The brightness temperature for a compact radio source is given by (e.g., [12])
(5)Tb=Iν10-29c22ν2kΩb,
where ν is the frequency, Iν is the peak intensity in mJy/beam, k is the Boltzmann constant, and Ωb is the solid angle of the beam given by (e.g., [15])
(6)Ωb=1.133Θb2,
where Θb is the angular resolution of the observations in radians.Finally, the optical depth (τ) is estimated using
(7)Tb=Te(1-e-τ).In order to obtain the physical parameters above, we assumed typical values for the electron temperature and abundance ofTe=104 K and Y=0.07, respectively. Using the equations above and the angular resolutions of Section 2, we obtain b(ν,Te)=0.7121 and Ωb=1.7×10-13 sr for the 1.3 cm image and b(ν,Te)=0.8025 and  Ωb=1.5×10-12 sr for the 3.6 cm image. The radius (ΘR) of the component A can be measured directly from Figures 1 and 2 and, thus, we can estimate relevant physical parameters for G75.78+0.34.In Table2 we present the physical parameters estimated by the equations above, which can be compared with previous estimates from the literature. The values obtained for the electron density are in reasonable agreement with those obtained by Wood and Churchwell [12] from the 6 cm radio emission (Ne=2.7×104 cm−3) and with the value obtained from 7 mm observations  -Ne≈5×104 cm−3 [16], as well as with the one found by Sánchez-Monge et al. [9] from a multifrequency study (Ne=3.7×104 cm−3). The emission measure found here is between the values found by Matthews et al. [17] of EM=1.1×106 cm−6 pc, by Wood and Churchwell [12] of EM=2.3×106 cm−6 pc, and by Sánchez-Monge et al. [9] of EM=2.5×107 cm−6 pc. Wood and Churchwell [12] found Tb=2300 K and τ=0.27, and thus, our values obtained from the 1.3 cm emission are in good agreement with theirs, while those estimated from the 3.6 cm are a bit smaller. The mass of G75.78+0.34 obtained here is about one order of magnitude smaller than the value found by Matthews et al. [17] and about one order of magnitude larger than the value obtained by Sánchez-Monge et al. [9], probably due to differences in the size of the region used to integrate the flux by these authors and by us, as well as due to the assumptions used in the calculations. The parameters presented in Table 2 confirm that G75.78+0.34 is an ultracompact H ɪɪ region [3], confirming previous results of Sánchez-Monge et al. [9].Table 2
Physical parameters obtained for the cometary HII region G75.78+0.34 from the 1.3 cm and 3.6 cm images.
Parameter
1.3 cm
3.6 cm
θ
R (arc sec)
0.9
1.2
N
e
(
cm
-
3
)
1.7
×
1
0
4
1.2
×
1
0
4
EM (cm-6pc)
7.6
×
1
0
6
5.1
×
1
0
6
M (M⊙)
2.5
×
1
0
-
2
3.9
×
1
0
-
2
T
b (K)
2530
1100
τ
0.29
0.12
Diameter (pc)
0.05
0.06For the components B and C, we estimate the physical parameters using only the 1.3 cm image, since it has the highest spatial resolution. For the component B, we obtainNe≈3.3×105 cm−3, EM≈1.9×107 cm−6 pc, and a mass of ionized gas of M≈1.6×10-3 M⊙, assuming a radius of 0.25 arcsec for the region. Assuming a radius of 0.4 arcsec for the component C, we obtain Ne≈1.6×105 cm−3, EM≈7.4×106 cm−6 pc, and M≈3×10-3 M⊙. These values are similar to those expected for ultracompact H ɪɪ regions [2, 3]. In fact, Sánchez-Monge et al. [9] identified the component C as being an ultracompact H ɪɪ region associated with dust emission in the millimetric and midinfrared wavelengths, while the component B seems to be embedded in dust.


## 4.2.  Molecular Gas

Although the signal-to-noise ratio of the HCO+ data was not high enough to construct flux and channel maps, as it has been done for the HCN in Riffel and Lüdke [7] using the same data, its detection can tell us some information about the star forming region G75.78+0.34. The complex line profile shown in Figure 3 suggests that the HCO+ emission originate from gas with a disturbed kinematics and since it usually originate from high density gas, the HCO+ emission may be tracing also the bipolar molecular outflows observed in HCN for G75.78+0.34 in our previous paper. A similar conclusion has been presented for the Serpens star forming region using BIMA observations by Hogerheijde [18], for which it is found that the HCN and HCO+ present enhanced emission near outflows, while the N2H+ reflects the distribution of the cloud.


### 4.2.1. SEST Observations and The Nondetection of SiO Emission

Besides the BIMA data, we have also employed the Swedish-ESO Submillimeter Telescope (SEST) in 20th April 2003 in order to detect higher excitation lines like SiO (2-1 at 86.646 GHz), SiO (3-2 at 130.268 GHz), SiO (5-4 at 217.104 GHz), and SiO (8-7, 347.330 GHz) to make a spectral line survey of maser emission from G75.78+0.34 and G75.77+0.34 at higher excitations. Even with longer integration times of about one hour per transition, we were unable to detect these lines at a confidence better than 5σ above the instrumental noise level.On the other hand, the H13CN at 86.338 GHz was present in our SEST observations, presenting a profile similar to the one of the HCN (1-0) suggesting that the emission may occur within zones of similar physical and kinematical conditions. Our observations therefore suggest that SiO lines may not be good observational tracers of shock-driven outflows in G75.78+0.34.This conclusion is supported in a similar result obtained for the star forming core W3-SE using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by Zhu et al. [19], in which the authors report the detection of the HCO+ associated with outflows, while the SiO (2-1) line at 86.243 GHz was also not detected for W3-SE in independent observations. This certainly brings the fact that there are difficulties in using SiO to obtain information on the astrophysical conditions of this compact object within the production of SiO by destruction of dust grains by radiatively driven MHD shock front from young and massive stars.On the other hand, we must emphasize that there are several works for UCH ɪɪ regions and more evolved objects showing that the SiO is a good tracer of outflows (e.g., [20–22]) and a possible explanation for the absence of excited SiO lines in G75.78+0.34 could be due to low sensitivity of the SEST observations. New and more sensitivity observations are henceforth needed to better constrain the SiO emission or its absence in G75.78+0.34 and to unravel such apparently contradictory statements.


## 4.2.1. SEST Observations and The Nondetection of SiO Emission

Besides the BIMA data, we have also employed the Swedish-ESO Submillimeter Telescope (SEST) in 20th April 2003 in order to detect higher excitation lines like SiO (2-1 at 86.646 GHz), SiO (3-2 at 130.268 GHz), SiO (5-4 at 217.104 GHz), and SiO (8-7, 347.330 GHz) to make a spectral line survey of maser emission from G75.78+0.34 and G75.77+0.34 at higher excitations. Even with longer integration times of about one hour per transition, we were unable to detect these lines at a confidence better than 5σ above the instrumental noise level.On the other hand, the H13CN at 86.338 GHz was present in our SEST observations, presenting a profile similar to the one of the HCN (1-0) suggesting that the emission may occur within zones of similar physical and kinematical conditions. Our observations therefore suggest that SiO lines may not be good observational tracers of shock-driven outflows in G75.78+0.34.This conclusion is supported in a similar result obtained for the star forming core W3-SE using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by Zhu et al. [19], in which the authors report the detection of the HCO+ associated with outflows, while the SiO (2-1) line at 86.243 GHz was also not detected for W3-SE in independent observations. This certainly brings the fact that there are difficulties in using SiO to obtain information on the astrophysical conditions of this compact object within the production of SiO by destruction of dust grains by radiatively driven MHD shock front from young and massive stars.On the other hand, we must emphasize that there are several works for UCH ɪɪ regions and more evolved objects showing that the SiO is a good tracer of outflows (e.g., [20–22]) and a possible explanation for the absence of excited SiO lines in G75.78+0.34 could be due to low sensitivity of the SEST observations. New and more sensitivity observations are henceforth needed to better constrain the SiO emission or its absence in G75.78+0.34 and to unravel such apparently contradictory statements.


## 5. Conclusions

We studied the radio continuum and molecular emission from the star forming region G75.78+0.34 using VLA and BIMA observations. Our main conclusions are as follows.(i)
The 3.6 and 1.3 cm radio continuum images for the H ɪɪ region G75.78+0.34 present three components, one associated with the cometary H ɪɪ region, other located at 6′′ east of the cometary H ɪɪ region, and another structure located at 2′′ south of it.(ii)
The cometary H ɪɪ region presents an electron density of≈1.5 × 104 cm−3, an emission measure of ≈6 × 107 cm−6 pc, ionized gas of ≈3 M⊙, and a diameter of 0.05 pc, consistent with the values expected for an ultracompact H ɪɪ region.(iii)
The HCO+ (J = 1-0) seems to originate from the gas which follows the same astrophysical conditions of outflows previously observed in main HCN transitions. Nevertheless, new interferometric observations with enhanced sensitivity and resolution are needed to better constraint the HCO+ origin in G75.78+0.34.(iv)
The SiO higher transitions up to 200 GHz were not detected using single dish observations with SEST of G75.78+0.34, suggesting that either it is not a good tracer of outflows in dense cores or that more sensitivity is needed at those relevant frequencies.



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*Source: 192513-2014-01-22.xml*