A&A 458, L21-L24 (2006)
DOI: 10.1051/0004-6361:20066161
LETTER TO THE EDITOR
F. Comerón1 - B. Reipurth2
1 - European Southern Observatory, Karl-Schwarzschild-Strasse 2,
85748 Garching bei München, Germany
2 - Institute for Astronomy, University of
Hawaii, 640 N. Aohoku Place, Hilo, HI 96720, USA
Received 1 August 2006 / Accepted 6 September 2006
Abstract
We report the discovery of a small bipolar Herbig-Haro
jet, HH 872, powered by the low-luminosity source
ESO-H 574 in Chamaeleon I. The end-to-end projected size
of the jet in [SII] images is only 3150 AU. Infrared images
marginally resolve the central source showing a structure
elongated perpendicularly to the jet axis, possibly a disk seen at
a large angle with respect to the plane of the sky. The brightest
feature of the jet, peaking at a distance of 1''6 from the
central source, is likely to result from enhanced outflow activity
in the last decade.
Key words: stars: low-mass, brown dwarfs - stars: pre-main sequence - ISM: jets and outflows
Increasing evidence suggests that the signposts of accretion that characterize the T Tauri phase among solar-type stars extend well into the substellar realm (see e.g. Luhman et al. 2006 for a recent review) and even into the giant-planet-mass domain (Muzerolle et al. 2005; Mohanty et al. 2005), bearing important constraints on the properties of their circum(sub)stellar disks (Alexander & Armitage 2006). Recent observations have also revealed outflow signatures around very low-mass stars and brown dwarfs (Fernández & Comerón 2001, 2005; Barrado y Navascués et al. 2004; Luhman 2004b; Whelan et al. 2005, 2006; Scholz & Jayawardhana 2006).
Recent surveys covering virtually the entire Chamaeleon I
star-forming clouds (Comerón et al. 2004;
Luhman 2004a; López Martí et al. 2004)
have revealed many new very low-mass stars and brown dwarfs. Among
them, Comerón et al. (2004) reported the existence of
a very faint source, ESO-H 574, with the
colors of lightly reddened late-type stars and a rich
emission-line spectrum dominated by the forbidden lines associated
with outflows. Lines normally used as accretion diagnostics, such as
HeI and CaII, are by comparison weak or absent. Comerón et
al. (2004) proposed that ESO-H
574 may be a
low-mass star with a strongly-veiled spectrum seen in scattered
light due to an edge-on disk blocking our direct view of the
photosphere of the central object. This may explain its low
luminosity (
), which taken at face value would place
the object below the main sequence. In this paper we report the
discovery of a well-developed jet, here designated HH 872,
detected in [SII] imaging of ESO-H
574, whose further study
can yield important clues to the validity of this scenario.
Our [SII] observations were carried out in Service Mode using the
visible imager and low resolution spectrograph FORS1 at the ESO Very
Large Telescope (VLT) on the night of 21 July 2005. The -band
imaging was obtained with ISAAC, the infrared camera and
low-resolution spectrograph at the VLT, also in Service Mode on the
night of 26 March 2005. The field around ESO-H
574
(
,
)
was observed with a [SII] filter, centered on 6728 Å and
with a full-width at half maximum (FWHM) of 66 Å. The filter
response is approximately uniform within an interval only slightly
narrower than the FWHM of the filter. Two exposures of 15 min each
were obtained under good seeing conditions yielding a quality of 0''70 on the combined image. The ISAAC
observation was a set
of
s exposures with small telescope offsets of 15''amplitude in between. We used the pipeline-reduced images of both
observations in the data set delivered to us (Silva &
Péron 2004).
An approximate calibration of the [SII] flux was carried out taking
the existing -band images of the field (Comerón et al. 2004) as a reference. The
magnitudes of the
stars in that field were converted to flux per unit wavelength
,
using
(Bessell 1979) and
assuming that
for those stars, given
the proximity in central wavelengths of the
and [SII] filters.
The total flux
within the window defined by the
[SII] transmission curve was then approximated by
,
where
is the FWHM of
the [SII] filter. Dividing the
thus derived for each
star by the analog-to-digital units (ADU) recorded in the detector
allowed us to obtain the conversion factor needed to transform ADUs
into power received from the source per unit surface. Since we lack
images sampling the continuum adjacent to the [SII] lines, we cannot
separate the contribution to the flux received within the [SII] filter window from the stellar photosphere and from the line
emission at the position of the central source of ESO-H
574.
Outside the central source we assume that the [SII] emission is much
more intense than any possible contribution to the continuum, such
as possible scattered light from the source.
![]() |
Figure 1:
Image of the field around ESO-H![]() |
Open with DEXTER |
The [SII] image of ESO-H 574 (Fig. 1) shows a
well-developed jet, HH 872, extending towards the northeast that can
be traced out to a distance of 11''3 from the central source. A
much fainter jet can be seen towards the southwest reaching out to a
distance of about 8''3. The northeastern jet is composed of four
distinct knots, as indicated in Fig. 2: the brightest
one, knot A, stretches 1''6 from the star, with a peak surface
brightness of
erg cm-2 s-1 arcsec-2. It is highly
reminiscent of HH 600, a knot in H
and [SII] images
of Par-Lup3-4 reported by Fernández &
Comerón (2005). A second component, knots B and C,
is
3'' away, knot C being the brightest with a surface
brightness of
erg cm-2 s-1 arcsec-2. The jet ends in the
distinct, faint knot D separated from the knot C by a gap of another
3''. The structure in the fainter southwestern jet is less
obvious, with a peak surface brightness
erg cm-2 s-1 arcsec-2 in knot E. The total
flux of HH 872 is estimated as
erg cm-2 s-1, excluding the flux unresolved from
the central source, which as explained in Sect. 2
cannot be disentangled from the photospheric continuum. At the
160 pc distance of the Chamaeleon I cloud (Wichmann et al. 1998), the luminosity in the [SII] lines is
,
and the projected end-to-end
length of HH 872 is 3140 AU (0.015 pc).
![]() |
Figure 2:
Contour plot of the central
![]() |
Open with DEXTER |
![]() |
Figure 3:
Contour plot of the ![]() ![]() ![]() ![]() |
Open with DEXTER |
No trace of HH 872 is seen in the image
(Fig. 3). However, the image quality (0''78 in the
final combined image) allows us to marginally resolve the central
source, which appears slightly elongated in the northwest-southeast
direction, roughly perpendicular to the jet. The estimated size of
the source, obtained from the quadratic difference between the major
and minor axes of the image of the source, respectively, and the
FWHM of the images of unresolved sources in the field, is
(
AU).
The
photometry of ESO-H
574 is
presented in Comerón et al. (2004). Unfortunately, its
location in the external parts of the Chamaeleon I cloud has
excluded it from observations of Chamaeleon I currently being
carried out by the Spitzer Space Telescope. There is, however, a
tentative IRAS detection at 100
m near its position, which may
be due to cold circumstellar material.
![]() |
Figure 4:
Spectrum of ESO-H![]() |
Open with DEXTER |
We can crudely estimate some physical characteristics of HH 872
by using line ratios from the spectrum of ESO-H 574
presented by Comerón et al. (2004) and by assuming
them to be representative of the entire jet. The spectrum
(Fig. 4) samples only the base of the jet, where other
contributions to H
may be expected, most notably accretion.
Therefore, both the
and
the
ratios are expected
to be lower limits to the ratios encountered along the jet. With
this caveat, we have applied the analysis of Bacciotti et
al. (1995). Assuming solar abundances, we obtain an
electron temperature
K and a hydrogen ionization
fraction x = 0.25. The electron density, from the
ratio, is
cm-3(Osterbrock 1989). Assuming that the measured
ratio is approximately the same
as the ratios between the [SII] and H
luminosities over the
entire jet, we obtain
.
Taking into account that these are conditions at
the base of the jet and that we have most likely underestimated
and
,
the average xand
in the jet are likely to be lower, and
higher. Nevertheless, the limits found on
,
x, and
are
similar to the values determined in other, much better-studied
T Tauri jets (e.g., Podio et al. 2006).
Estimates of the expected H
luminosity
of the shock-bounded internal working surfaces of brown dwarf-driven
jets have been provided by Masciadri & Raga (2004).
Assuming that the approximate proportionality between mass loss and
accretion rate in T Tauri stars (Hartigan et al. 1995)
holds for brown dwarfs, and considering the rough proportionality
between the accretion rate and the square of the mass of the central
object (Muzerolle et al. 2005), the relationship
between
and the mass-loss rate in the jet suggests
that jets powered by brown dwarfs must be typically two orders of
magnitude fainter than those powered by solar-type T Tauri stars. In
the case of the HH 872, the scenario worked out by Masciadri &
Raga (2004) is most likely found in knot A, where the
freshly ejected gas from the star first encounters slower moving gas
ejected earlier.
Our estimate of
for this segment is in principle in better
agreement with Masciadri & Raga's prediction for a brown
dwarf-powered jet than for a classical T Tauri-driven jet. We must
nevertheless note the large scatter in the accretion rate vs.
central mass relationship (Luhman et al. 2006),
consequently resulting in a large scatter in
at a
given central mass stemming from this reason alone. Furthermore,
scales with the third power of the shock velocity,
which is in turn related to the time variability of the jet, making
very sensitive to it. Finally, as noted above, our
own estimate of
is indirect and considerably
uncertain. Therefore, although the inferred
hints
at ESO H
574 being a very low-mass star or brown dwarf,
model predictions are far too uncertain, given the lack of direct
knowledge of the quantities involved, to rule out a more massive
central source.
The 11''3 angular extent of the northeastern jet corresponds to a
projected 0.009 pc at the distance of 160 pc.
The jet ejection velocity is unknown but is expected to be of the
order of the escape velocity of the central object, which for young
objects is little sensitive to their mass since M / R varies
little over the range from solar-type stars to low-mass brown
dwarfs. Assuming a projected jet velocity of 100 km s-1 the
dynamical timescale is of order of 100 years, and the brightest
segment at the base of the northeastern jet may thus result from a
mass loss episode having started only about a decade ago. With 4 knots in the northeastern jet, the mean mass-loss variability
timescale is 25 years. However, given the large variations
found among individual jets (e.g. velocities in the
300-600 km s-1 range are observed in the HH 111 jet; Reipurth
et al. 1997), these quantities are just indicative.
A high-sensitivity survey of most of the Chamaeleon I cloud
searching for [SII] emission has been recently presented by Wang &
Henning (2006), who report 14 new Herbig-Haro objects and
detailed observations of the previously known HH 48 to HH 50. Three of the new objects have a jet morphology, with
the others appearing as knots or patches. ESO-H 574, located
in the northeastern outskirts of the Chamaeleon I North cloud, was
slightly outside their surveyed area. The peak surface brightness of
HH 872,
erg cm-2 s-1 arcsec-2,
is similar to the typical brightness of the objects observed by Wang
& Henning (2006). However, none of the [SII]-emitting
features reported by Wang & Henning displays the compact jet
structure and the unambiguous association with its central source of
HH 872. Moreover, the distances to their exciting sources, in the
cases where the latter can be identified, are always much larger
than the size of HH 872 jet, including the three instances
(HH 51, HH 909, and
HH 908-HH-910) in which the suspected exciting
sources are either very low-mass stars or brown dwarfs.
The discovery of HH 872, an optical jet powered by
ESO-H 574, is perhaps not surprising given the previous
detection of strong outflow signatures in the spectrum of the
central source (Comerón et al. 2004). The limited
information available thus far allows us to obtain crude estimates
of the electron density, temperature, and ionization fraction in the
jet, which are similar to those of jets excited by T Tauri stars.
The morphology of the central source, which is barely resolved in
the
band, indicates a flattened structure elongated in the
direction perpendicular to the jet, suggesting a disk viewed at a
large angle from the pole-on direction. In this regard
ESO-H
574 may be similar to LkH
263C, a
young stellar object discovered by Jayawardhana et
al. (2002) in MBM 12 with an estimated
spectral type of M0 and a well-resolved nearly edge-on disk. The
spectrum of LkH
263C also displays emission lines
characteristic of outflows, although with a lower intensity that
suggests that its possible jet, as yet undetected, should be much
less prominent than the one reported here. On the other hand, our
observations rule out an edge-on disk as extended as that around
LkH
263C, as the estimated physical size of the central
source is roughly five times smaller than that reported by
Jayawardhana et al. (2002).
The properties of the jet do not provide a definitive answer as to the
nature of the central source. In particular, the question of whether
or not the faintness of ESO-H 574 may actually be due to
blocking by a circumstellar disk remains open. Nevertheless, both
the low luminosity estimated for the internal working surface
closest to the star and the small overall size of the structure
hint at a very low mass of the central source. Assuming a
jet-ejection velocity of
100 km s-1, the length scale of
the features in HH 872 implies the record of the mass ejection
history of the source during the past century, and the brightest
part of the jet, reaching only 1''6 from the central object, may
be the result of a mass loss outburst having developed over the past
decade. More observations, in particular high-resolution
spectroscopy along the jet, yielding accurate line ratios and
kinematics, and monitoring of the evolution of HH 872 over a
timescale of a few years, will be needed to better characterize the
properties of the jet and to constrain those of the central source.
However, the tentative conclusions presented here already suggest
that ESO-H
574 is a good candidate for being one of the
lowest mass sources known to power a Herbig-Haro outflow, opening
the door to the detailed observational study of jets near the end of
the stellar mass spectrum or possibly beyond.
Acknowledgements
We thank the ESO staff on Cerro Paranal who carried out the Service Mode observations, the ESO User Support Department for their valuable assistance in the preparation of our observations, and the ESO Data Flow Operations Group for the preparation of our data package. We also appreciate the comments of the referee, Ray Jayawardhana, pointing out the possible similarity between ESO-H
574 and LkH
263C.