EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 602 (June 2017) A&A, 602 (2017) L2 Full HTML
Free Access
Issue
A&A
Volume 602, June 2017
Article Number L2
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201730732
Published online 31 May 2017

© ESO, 2017

1. Introduction

Observations suggest the gravitational collapse of the gas within young clusters as a key ingredient determining the dynamical properties of these systems. In a recent work, Kirk et al. (2013) investigated the presence of gravitationally-induced motions in the Serpens-South region. From the analysis of the N2H+ emission as unambiguous tracer of the dense, UV-shielded molecular gas (Pety et al. 2017), Kirk et al identified a longitudinal velocity gradient as part of the filamentary accretion inflow toward this proto-cluster. Peretto et al. (2014) attributed the detection of similar linear gradients to the homologous collapse along filaments feeding the central clump of the SDC13 infrared dark cloud. Increasing evidence indicates that these gravitationally dominated accretion flows might also be involved in the formation of massive stars (e.g., Galván-Madrid et al. 2010; Peretto et al. 2013).

If generated by a free-fall collapse, gravity is expected to produce a characteristic signature on the gas velocity structure. Due to the radial dependency of the gravitational attraction, models of clouds in gravitational collapse (e.g., Gómez & Vázquez-Semadeni 2014) predict these motions to be accelerated towards the center of the potential well. Despite these expectations, such gravitationally driven accelerations remain poorly characterized in observations.

In this Letter, we investigate the dynamical state of the dense gas along the integral shaped filament (ISF) in Orion (Johnstone & Bally 1999). As illustrated in Fig. 1, the ISF harbors the Orion Nebula Cluster (ONC), the most active stellar cluster in the solar neighborhood and the nearest site for high-mass star formation, including the Trapezium stars and the Orion KL region (see O’dell 2001, for a review). Still partially embedded in the ISF, the ONC is found in association with large amounts of dense material within OMC-1 cloud, a region widely investigated in the past at millimeter wavelengths (e.g., Martin-Pintado et al. 1990; Rodriguez-Franco et al. 1992; Wiseman & Ho 1998). Our results demonstrate the presence of accelerated gas motions along the OMC-1 cloud consistent with the expected gravitational collapse of this region.

2. IRAM 30 m observations

thumbnail Fig. 1

From left to right: a) VISTA-NIR image of the ISF (Meingast et al. 2016); b) IRAM 30 m integrated N2H+ (1−0) emission; c) N2H+ line velocity centroid (VLSR) and d) N2H+ Full-Width-Half-Maximum (FWHM) as a function of declination. Map offsets are referred, in radio projection, to the position of the Orion BN source (α,δ)J2000=(05h35m14.s2,−05◦22′21′′)\hbox{$(\alpha,\delta)_{\rm J2000} = (\rm 05^h35^m14\fs2,-05{\circ}22'21'')$} (white cross). N2H+ contours are equally spaced every 2 K km s-1. For reference, the first N2H+ contour is superposed to the IR image. The location of the most prominent molecular fingers (e.g., the OMC-1 ridge, MF3, and HVF; Rodriguez-Franco et al. 1992) are indicated by red lines in the integrated intensity map. The magnitude of representative gradients with 1 (green) plus 5, and 7 (blue) km s-1 pc-1 are indicated in the velocity plot. The position of the OMC-1 South clump with the most blue-shifted velocity is indicated in both maps (green cross) and kinematic plots (green dashed line).

We observed the entire ISF in November 2013 using the IRAM 30 m telescope. We observed this region at the frequency of the N2H+ (1−0) line (93173.764 MHz, Pagani et al. 2009) using the EMIR receiver connected to the VESPA spectrometer achieving an effective spectral resolution of 0.06 km s-1. The observations were carried out in Position-Switching mode using an OFF position at approximately 1 degree from the center of our maps with no detected emission above 0.02 K. Calibrations were carried out every 15 min as well as pointing and focus every 1.5−2.0 h. The reduction strategy, baseline subtraction, and main beam calibration follow the reduction scheme presented by Hacar et al. (2017). Our final map covers a total area of ~420 arcmin2 obtained from a mosaic with different tiles of 200 × 200 and 100 × 100 arcsec2 each. A final Nyquist sampled set of 7030 spectra are obtained after the convolution of the original dataset into a final resolution of 30′′, showing a typical rms of 0.15 K. All the data presented in this work will be released after their combination with existing interferometric observations (Hacar, et al., in prep.).

Figure 1b illustrates the total integrated intensity map of the N2H+ (1−0) emission within this region. The coverage of our maps corresponds to a ~7-pc long, north-south longitudinal cut along the entire ISF, including the ONC (e.g., O’dell 2001), the Orion BN/KL region, the Orion Bar, and the Orion HII region around the Trapezium (e.g., Goicoechea et al.2015; see also Fig.1a). Tracing the gas at densities of n(H2) > 104.5 cm-3 (e.g., Caselli et al. 2002), the N2H+ emission reveals the intricate distribution of dense gas along the main spine of the ISF. Several branches and substructures are identified in regions like OMC-2/3, in agreement with previous results (e.g., Li et al. 2013). Additional features, such as the molecular fingers (Martin-Pintado et al. 1990; Rodriguez-Franco et al. 1992) and the OMC-1 South region (Mezger et al. 1990) are clearly distinguished by their bright N2H+ emission. Disconnected from the rest of the cloud, the emission of this molecule is recovered towards the south, coincident with the OMC-4 region. The distribution of the N2H+ (1−0) emission in our maps is in good agreement with previous studies in the same region (Tatematsu et al. 2008). Compared to these observations, however, our data is more sensitive and is better spectrally and spatially resolved by a factor of 1.5−2.

3. Accelerated gas motions towards the ONC

We investigated the internal gas motions in the ISF from the detailed analysis of the N2H+ (1−0) emission profiles. This information is obtained from the hyperfine fit of the individual spectra following the same multi-line fitting strategy presented by Hacar et al. (2017). This fitting procedure provides a full description of the gas emission in terms of the mean gas velocity along the line-of-sight (i.e., velocity centroids), the FWHM, line emission properties (i.e., intensity and opacity), and line multiplicity (or number of components) at each position in our map.

Using the above fitting procedure, we recover a total of 4207 components with S/N ≥ 3. At the angular resolution of our single-dish observations, a large fraction of the spectra present a single line component. Nevertheless, extended areas exhibiting well-separated, double peaked spectra are found in regions like the OMC-1 ridge and the OMC-4 cloud. Due to the limited beam size of our IRAM 30 m observations, in this work we restrict our study to the gas motions within the ISF at scales ≳0.25 pc. The internal physical and kinematic substructure of this region will be investigated in higher detail in a subsequent paper combining both the current single-dish observations and a new set of ALMA interferometric data (Hacar et al., in prep.).

Figure 1c shows the mean velocity of the gas along the line-of-sight (VLSR) as a function of declination for all the detected components in our maps (red points). Previous studies using observations of different CO isotopologs have pointed out the existence of a global north-south velocity gradient of ≲1 km s-1 pc-1 in ISF (green line; Bally et al. 1987) continuing along the entire Orion A cloud (Hacar et al. 2016). A similar trend is observed in the dense gas detected in N2H+ at large scales, with velocities ranging between VLSR ~ 11.5 km s-1 in OMC-3 and ~8 km s-1 in OMC-4.

In addition to the above global gradient, Fig. 1c reveals a rapid change of the gas velocities in the proximity of the ONC region. The observed N2H+ emission exhibits a strong blue-shifted drift towards the OMC-1 cloud. Similar gas motions have been suggested from the analysis of the gas kinematics along the main axis of the OMC-1 gas molecular fingers (Rodriguez-Franco et al. 1992; Wiseman & Ho 1998).

When observed at large scales, the velocity structure within the OMC-1 cloud describes a characteristic V-shape centered around the OMC-1 South clump. In the proximity of the ONC, we identify gradient values up to 5−7 km s-1 pc-1 (blue lines), that is, between 5−10 times larger than those values measured in other regions of the same complex, such as OMC-2 or OMC-3. The systematic nature of these motions indicates that the gas is accelerated in the directions of the OMC-1 region.

4. Radial dependency of the gas motions within the OMC-1 region

thumbnail Fig. 2

Gas velocity structure as a function of the distance to the OMC-1 South cloud for all the gas components detected with S/N ≥ 3 (gray squares). Different lines describe the expected velocity profile for a free-falling particle in a series of potential wells with different masses M observed at different angles α following Eq. (1) (see parameters in the lower right corner; masses are in M⊙ and angles are in degrees).

The blue-shifted velocity feature identified in Fig. 1 appears to present a radial dependence respect to the position of the OMC-1 South clump. We have highlighted this behavior in Fig. 2 by plotting the gas velocity structure as a function of the distance to coordinates (x,y) = (45′′, −120′′) in our maps, selected as the position of most blue-shifted line centroid within the OMC-1 region. As deduced from this plot, the reported velocity gradient extends radially across the entire OMC-1 region and up to distances of ~400 arcsec from this central position, or ~0.8 pc at the distance of Orion (D = 414 pc, Menten et al. 2007).

Although less systematic than the velocity shifts detected in the line centroids, a similar radial dependency is observed between the derived N2H+ FWHM as a function of the distance to the OMC-1 South region (see Fig. 1d). In relative terms, the observed FWHM rises from approximately 0.5−1.0 km s-1 in regions like OMC-2 or OMC-4 to up to 2.5−3.0 km s-1 in the area surround the OMC-1 South cloud. Part of these effects can be explained by thermal broadening effects in the proximity of the Trapezium stars produced by the increasing gas temperatures measured in this region (Wiseman & Ho 1998). In addition to this, the parallel evolution of the observed FWHM with the gas velocity gradients suggests that part of the reported enhanced FWHM values could be generated by the increasing contribution of the large-scale motions on the velocity field sampled along the line-of-sight (l.o.s.).

Interestingly, the direction of the gas velocity gradients within the OMC-1 region closely corresponds with the direction of the well characterized molecular fingers (Rodriguez-Franco et al. 1992; Wiseman & Ho 1998). When isolated by their integrated emission, the gas velocity field along each of these structures describes a continuous velocity track as a function of radius with remarkably small deviations from their large-scale behavior (e.g., MF3 or HVF in Rodriguez-Franco et al. 1992, see also Fig. 1b). With perhaps the exception of the more complex OMC-1 ridge, the systematic organization of the observed physical and kinematic structrure of the gas at large scales might explain the origin of the molecular fingers within the OMC-1 region.

5. Gravitational collapse of OMC-1 region

The characterization of the line centroid of molecular lines and, in particular, their Doppler velocities provide information on the bulk motions of the gas along the l.o.s.. Due to the lack of information about the real 3D-space, however, the physical interpretation of the relative motions between superposed structures usually lead to ambiguous conclusions. Depending on their relative orientation, the observational detection of velocity gradients and/or velocity differences can be equally interpreted as both converging or diverging motions (e.g., see Fig. 12 in Henshaw et al. 2014).

Similar to our results, the presence of a blue-shifted, V-shape velocity structure of the dense gas associated ONC was first reported by Rodriguez-Franco et al. (1992) from the study of the HC3N emission within the OMC-1 cloud. From the comparison with lower density tracers, Rodriguez et al. suggested that the gas molecular fingers are produced by the interaction of the ionized and neutral gas. In particular, these authors interpret the abrupt variation of the gas velocity as the direct impact of the shock-front with the pre-existing dense gas in the area surrounding of the Trapezium region, producing a pillar-like structure showing a velocity shift respect to the outermost gas (see also Murata et al. 1990).

Different observables seem to be in tension with this sweep-up scenario. First, this pillar-like configuration should favor the formation of cometary shapes with characteristic head-tail enhancements, similar to those clumpy regions exposed to stellar winds, such as the Horsehead Nebula (e.g., Hily-Blant et al. 2005), not observed in any previous molecular dataset within this region. More importantly, it is unclear how this formation mechanism would mimic the velocity structure and continuity of the cloud at large scales in regions not affected by these winds (e.g., OMC-2/3; see Fig. 1c). Although some of the observed molecular fingers could indeed be shaped by the strong stellar feedback within the ONC region (e.g., OMC-1 South, O’dell 2001), winds alone seem an unlikely mechanism for the formation of these objects.

Alternatively, we suggest that the velocity gradient observed towards the OMC-1 region actually corresponds with dense gas material moving in the direction of the observer and towards the position of the ONC. The low extinction values measured toward the Trapezium region demonstrate that most of the dense gas detected along the OMC-1 ridge is located behind this stellar cluster (e.g., O’dell 2001). This particular configuration allows us to break the degeneracy: red-shifted gas velocities would then be interpreted as outflowing motions along the l.o.s. and moving away from the stars. On the other hand, the observed blue-shifted velocities would be indicative of infalling material towards the cluster center.

As a unique characteristic of gravitationally generated motions, a rapid acceleration is expected in the proximity of the potential well. It is easy to prove that for a point-like mass in free-fall, the observed l.o.s. velocity VLSR at a given impact parameter p can be described by the following relation: VLSR(p)=Vsys,0+Vinfall(p)·cos(α)\begin{equation} \label{eq:infall} V_{\rm LSR}(p)=V_{\rm sys,0}+V_{\rm infall}(p) \cdot \cos(\alpha) \end{equation}(1)where Vsys is the initial systemic velocity and Vinfall(p)=−2GMR=−2GMp/sinα\hbox{$V_{\rm infall}(p)=-\sqrt{\frac{2GM}{R}}=-\sqrt{\frac{2GM}{p\!{/}\!\sin \alpha}}$} the infall velocity in a potential of a mass M as a function of the distance R to its center, respectively, with α describing the orientation angle of these infalling motions with respect to the l.o.s.. In such configuration, the observed velocities are expected to present an approximately ~p− 1/2 functional dependence with respect to the center of the potential well, modulated by their viewing angle α.

In order to describe the global motions within the OMC-1 region, in Fig. 2 we display the expected velocity profiles for particles in free-fall in three potential wells with masses of 2250 (blue), 1500 (red), and 750 (green) M⊙, all of them presenting a systemic velocity Vsys,0 = 10.8 km s-1 similar to the observed gas velocities at the northern end of the OMC-1 region (see Fig. 1). In addition to this, we explore different projection angles α leading to reasonable fits of the observed gas velocities. In all cases, the kinematic signature of the gravitational infall is assumed to be blue-shifted with respect to the systemic velocity given the physical 3D configuration of this cloud (see above).

As seen in Fig. 2, our toy model closely reproduces most of the bulk motions observed along the OMC-1 region. We find remarkably good agreement between our fitting values and the measured masses for the ONC, estimated in ~1800 M⊙ (with a r0 ~ 0.2 pc, Hillenbrand & Hartmann 1998), assumed as the dominating component of the gravitational potential over the ≲600 M⊙ of gas detected within the same region (Goldsmith et al. 1997). Moreover, our models predict the molecular fingers to be oriented close to the plane of the sky (i.e., α ~ 55−80 deg), explaining their long projected dimensions observed at mm-wavelengths (e.g., Wiseman & Ho 1998). Deviations from this global behaviour can be explained by the intrinsically more complex structure of the OMC-1 region and the distinct orientation of each individual molecular finger compared to our oversimplified model. Still, the good agreement of the above results indicates that most of the accelerated motions identified within the OMC-1 region could actually correspond to the kinematic signature generated by its gravitational collapse.

6. Discussion and conclusions

In this letter we have investigated the global velocity structure of the ISF in Orion using a new series of IRAM 30 m N2H+ (1−0) observations. Compared to the smooth velocity gradients dominating the global velocity structure of this cloud, our large-scale maps demonstrate the presence of accelerated motions towards the OMC-1 region with gradients up to 7 km s-1 pc-1. When displayed in a Position-Velocity diagram, these motions exhibit a characteristic blue-shifted, V-shape centered at the position of the OMC-1 South.

The direction of the maximum gradients observed along the OMC-1 region seem to coincide with the orientation of the so-called molecular fingers. Although initially interpreted as ejected material, the large-scale continuity of these motions and the well characterized physical structure of this region suggest that the observed V-shaped profile may correspond to an accelerated material inflowing towards the ONC. The bulk of these motions, as well as their radial dependency, can be reproduced by a simplified infall model, whose physical properties mimic the expected mass, orientation, and 3D structure of the ONC region. We conclude that both the mass distribution and gas kinematic within the OMC-1 region might be dominated by the gravitational collapse of this cloud.

If confirmed, the proposed collapse of the OMC-1 region could potentially provide a significant mass accretion flow onto the ONC cluster. For a filamentary inflow, the mass accretion rate can be described by Ṁ = πr2⟨n(H2)⟩ × Vinfall(R) (e.g., see Kirk et al. 2013). Falling from a distance R = 0.8 pc (see Sect. 4), and with a typical radius of r ~ 0.05 pc and an average density ⟨n(H2)⟩ ~ 105 cm-3, the mass inflow per molecular finger is estimated in Ṁi ~ 55 M⊙ Myr-1. The 7 molecular fingers detected in OMC-1 (Rodriguez-Franco et al. 1992) would then contribute with a total Ṁ(total) ~ 385 M⊙ Myr-1.

Our results in the OMC-1 region provide new evidence indicating gravity as a key ingredient for the formation of massive clusters. Interestingly, the gravitational collapse of the OMC-1 region appears to continue after the formation of the main cluster core suggesting that the cluster assembling phase might expand on timescales of several Myr. In the particular case of the ONC, the still on-going collapse of the OMC-1 region could potentially explain the elongated, and still not relaxed, nature of this cluster. Moreover, the continuous inflow of fresh material contained in these star-forming molecular fingers brings a new perspective on the stellar mass segregation reported in previous studies (Hillenbrand & Hartmann 1998).

Acknowledgments

This work is part of the research programme VENI with project number 639.041.644, which is partly financed by the Netherlands Organisation for Scientific Research (NWO). MT and AH thank the Spanish MINECO for support under grant AYA2016-79006-P. JRG and MT thank the Spanish MINECO for support under grant AYA2012-32032.

References

  1. Bally, J., Langer, W. D., Stark, A. A., & Wilson, R. W. 1987, ApJ, 312, L45 [NASA ADS] [CrossRef] [Google Scholar]
  2. Caselli, P., Benson, P. J., Myers, P. C., & Tafalla, M. 2002, ApJ, 572, 238 [NASA ADS] [CrossRef] [Google Scholar]
  3. Johnstone, D., & Bally, J. 1999, ApJ, 510, L49 [NASA ADS] [CrossRef] [Google Scholar]
  4. Kirk, H., Myers, P. C., Bourke, T. L., et al. 2013, ApJ, 766, 115 [NASA ADS] [CrossRef] [Google Scholar]
  5. Hacar, A., Alves, J., Forbrich, J., et al. 2016, A&A, 589, A80 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  6. Hacar, A., Tafalla, M., & Alves, J. 2017, A&A, accepted, [arXiv:1703.07029] [Google Scholar]
  7. Henshaw, J. D., Caselli, P., Fontani, F., Jiménez-Serra, I., & Tan, J. C. 2014, MNRAS, 440, 2860 [NASA ADS] [CrossRef] [Google Scholar]
  8. Hillenbrand, L. A., & Hartmann, L. W. 1998, ApJ, 492, 540 [NASA ADS] [CrossRef] [Google Scholar]
  9. Hily-Blant, P., Teyssier, D., Philipp, S., & Güsten, R. 2005, A&A, 440, 909 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  10. Galván-Madrid, R., Zhang, Q., Keto, E., et al. 2010, ApJ, 725, 17 [NASA ADS] [CrossRef] [Google Scholar]
  11. Goicoechea, J. R., Teyssier, D., Etxaluze, M., et al. 2015, ApJ, 812, 75 [NASA ADS] [CrossRef] [Google Scholar]
  12. Goldsmith, P. F., Bergin, E. A., & Lis, D. C. 1997, ApJ, 491, 615 [NASA ADS] [CrossRef] [Google Scholar]
  13. Gómez, G. C., & Vázquez-Semadeni, E. 2014, ApJ, 791, 124 [NASA ADS] [CrossRef] [Google Scholar]
  14. Li, D., Kauffmann, J., Zhang, Q., & Chen, W. 2013, ApJ, 768, L5 [NASA ADS] [CrossRef] [Google Scholar]
  15. Martin-Pintado, J., Rodriguez-Franco, A., & Bachiller, R. 1990, ApJ, 357, L49 [NASA ADS] [CrossRef] [Google Scholar]
  16. Meingast, S., Alves, J., Mardones, D., et al. 2016, A&A, 587, A153 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  17. Menten, K. M., Reid, M. J., Forbrich, J., & Brunthaler, A. 2007, A&A, 474, 515 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  18. Mezger, P. G., Zylka, R., & Wink, J. E. 1990, A&A, 228, 95 [NASA ADS] [Google Scholar]
  19. Murata, Y., Kawabe, R., Ishiguro, M., et al. 1990, ApJ, 359, 125 [NASA ADS] [CrossRef] [Google Scholar]
  20. O’dell, C. R. 2001, ARA&A, 39, 99 [NASA ADS] [CrossRef] [Google Scholar]
  21. Pagani, L., Daniel, F., & Dubernet, M.-L. 2009, A&A, 494, 719 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  22. Peretto, N., Fuller, G. A., Duarte-Cabral, A., et al. 2013, A&A, 555, A112 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  23. Peretto, N., Fuller, G. A., André, P., et al. 2014, A&A, 561, A83 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  24. Pety, J., Guzmán, V. V., Orkisz, J. H., et al. 2017, A&A, 599, A98 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  25. Rodriguez-Franco, A., Martin-Pintado, J., Gomez-Gonzalez, J., & Planesas, P. 1992, A&A, 264, 592 [NASA ADS] [Google Scholar]
  26. Tatematsu, K., Kandori, R., Umemoto, T., & Sekimoto, Y. 2008, PASJ, 60, 407 [NASA ADS] [Google Scholar]
  27. Wiseman, J. J., & Ho, P. T. P. 1998, ApJ, 502, 676 [NASA ADS] [CrossRef] [Google Scholar]

All Figures

thumbnail Fig. 1

From left to right: a) VISTA-NIR image of the ISF (Meingast et al. 2016); b) IRAM 30 m integrated N2H+ (1−0) emission; c) N2H+ line velocity centroid (VLSR) and d) N2H+ Full-Width-Half-Maximum (FWHM) as a function of declination. Map offsets are referred, in radio projection, to the position of the Orion BN source (α,δ)J2000=(05h35m14.s2,−05◦22′21′′)\hbox{$(\alpha,\delta)_{\rm J2000} = (\rm 05^h35^m14\fs2,-05{\circ}22'21'')$} (white cross). N2H+ contours are equally spaced every 2 K km s-1. For reference, the first N2H+ contour is superposed to the IR image. The location of the most prominent molecular fingers (e.g., the OMC-1 ridge, MF3, and HVF; Rodriguez-Franco et al. 1992) are indicated by red lines in the integrated intensity map. The magnitude of representative gradients with 1 (green) plus 5, and 7 (blue) km s-1 pc-1 are indicated in the velocity plot. The position of the OMC-1 South clump with the most blue-shifted velocity is indicated in both maps (green cross) and kinematic plots (green dashed line).
In the text
thumbnail Fig. 2

Gas velocity structure as a function of the distance to the OMC-1 South cloud for all the gas components detected with S/N ≥ 3 (gray squares). Different lines describe the expected velocity profile for a free-falling particle in a series of potential wells with different masses M observed at different angles α following Eq. (1) (see parameters in the lower right corner; masses are in M⊙ and angles are in degrees).

In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.