49 research outputs found
Three dimensional maps of the Magellanic Clouds using RR Lyrae Stars and Cepheids II. The Small Magellanic Cloud
We use data on variable stars from the Optical Gravitational Lensing
Experiment (OGLE III) survey to determine the three-dimensional structure of
the Small Magellanic Cloud (SMC). Deriving individual distances to RR Lyrae
stars and Cepheids we investigate the distribution of these tracers of the old
and young population in the SMC. Photometrically estimated metallicities are
used to determine the distances to 1494 RR Lyrae stars, which have typical ages
greater than 9 Gyr. For 2522 Cepheids, with ages of a few tens to a few hundred
Myr, distances are calculated using their period-luminosity relation.
Individual reddening estimates from the intrinsic color of each star are used
to obtain high precision three-dimensional maps. The distances of RR Lyrae
stars and Cepheids are in very good agreement with each other. The median
distance of the RR Lyrae stars is found to be 61.5 +/- 3.4 kpc. For the
Cepheids a median distance of 63.1 +/- 3.0 kpc is obtained. Both populations
show an extended scale height, with 2.0 +/- 0.4 kpc for the RR Lyrae stars and
2.7 +/- 0.3 kpc for the Cepheids. This confirms the large depth of the SMC
suggested by a number of earlier studies. The young population is very
differently oriented than the old stars. While we find an inclination angle of
7{\deg} +/- 15{\deg} and a position angle of 83{\deg} +/- 21{\deg} for the RR
Lyrae stars, for the Cepheids an inclination of 74{\deg} +/- 9{\deg} and a
position angle of 66{\deg} +/- 15{\deg} is obtained. The RR Lyrae stars show a
fairly homogeneous distribution, while the Cepheids follow roughly the
distribution of the bar with their northeastern part being closer to us than
the southwestern part of the bar. Interactions between the SMC, LMC, and Milky
Way are presumably responsible for the tilted, elongated structure of the young
population of the SMC.Comment: 13 pages, 6 figures, 4 tables, published in A
Halo Velocity Groups in the Pisces Overdensity
We report spectroscopic observations with the Gemini South Telescope of 5
faint V~20 RR Lyrae stars associated with the Pisces overdensity. At a
heliocentric and galactocentric distance of ~80 kpc, this is the most distant
substructure in the Galactic halo known to date. We combined our observations
with literature data and confirmed that the substructure is composed of two
different kinematic groups. The main group contains 8 stars and has =
50 km/s, while the second group contains four stars at a velocity of
= -52 km/s, where V_{gsr} is the radial velocity in the galactocentric standard
of rest. The metallicity distribution of RR Lyrae stars in the Pisces
overdensity is centered on [Fe/H]=-1.5 dex and has a width of 0.3 dex. The new
data allowed us to establish that both groups are spatially extended making it
very unlikely that they are bound systems, and are more likely to be debris of
a tidally disrupted galaxy or galaxies. Due to small sky coverage, it is still
unclear whether these groups have the same or different progenitors.Comment: 21 pages, 5 figures, 3 tables, accepted to Astrophysical Journa
A fork in the Sagittarius trailing debris
We take advantage of the deep and wide coverage of the VST ATLAS survey to
study the line-of-sight structure of the Sagittarius stellar stream in the
Southern hemisphere, only ~40{\deg} away from the progenitor. We use
photometrically selected Sub-Giant Branch (SGB) stars to reveal a complex
debris morphology of the trailing arm and detect at least two clear peaks in
the SGB distance modulus distribution. The separation between the two
line-of-sight components is at least 5 kpc at the edge of the VST ATLAS
footprint, but appears to change along the stream, which allows us to conclude
that these detections correspond to two physically independent stellar
structures, rather than a mix of co-distant stellar populations within a single
stream. Our discovery of a fork in the Sgr trailing arm is verified using Blue
Horizontal Branch stars and our distance measurements are calibrated using RR
Lyrae stars from the Catalina Real-Time Transient Survey. Comparing with
numerical simulations of the Sgr dwarf disruption, the more distant of the two
components in the fork matches perfectly with the track of the trailing debris.
However, no obvious counterpart exists in the simulation for the closer
line-of-sight component.Comment: 15 pages, 12 figures, accepted for publication in MNRA
Spectroscopy of Bright QUEST RR Lyrae Stars: Velocity Substructures toward Virgo
Using a sample of 43 bright (V<16.1, distance <13 kpc) RR Lyrae stars (RRLS)
from the QUEST survey with spectroscopic radial velocities and metallicities,
we find that several separate halo substructures contribute to the Virgo
overdensity (VOD). While there is little evidence for halo substructure in the
spatial distribution of these stars, their distribution in radial velocity
reveals two moving groups. These results are reinforced when the sample is
combined with a sample of blue horizontal branch stars that were identified in
the SDSS, and the combined sample provides evidence for one additional moving
group. These groups correspond to peaks in the radial velocity distribution of
a sample of F type main-sequence stars that was recently observed in the same
directon by SEGUE, although in one case the RRLS and F star groups may not lie
at the same distance. One of the new substructures has a very narrow range in
metallicity, which is more consistent with it being the debris from a destroyed
globular cluster than from a dwarf galaxy. A small concentration of stars have
radial velocities that are similar to the Virgo Stellar Stream (VSS) that was
identified previously in a fainter sample of RRLS. Our results suggest that
this feature extends to distances as short as ~12 kpc from its previous
detection at ~19 kpc. None of the new groups and only one star in the sample
have velocities that are consistent with membership in the leading tidal stream
from the Sagittarius Dwarf Spheroidal Galaxy, which some authors have suggested
is the origin of the VOD.Comment: Accepted for publication in the A
Stellar streams around the Magellanic Clouds in 4D
We carried out a spectroscopic follow-up program of the four new stellar
stream candidates detected by Belokurov & Koposov (2016) in the outskirts of
the Large Magellanic Cloud (LMC) using FORS2 (VLT). The medium-resolution
spectra were used to measure the line-of-sight velocities, estimate stellar
metallicities and to classify stars into Blue Horizontal Branch (BHB) and Blue
Straggler (BS) stars. Using the 4-D phase-space information, we attribute
approximately one half of our sample to the Magellanic Clouds, while the rest
is part of the Galactic foreground. Only two of the four stream candidates are
confirmed kinematically. While it is impossible to estimate the exact levels of
MW contamination, the phase-space distribution of the entire sample of our
Magellanic stars matches the expected velocity gradient for the LMC halo and
extends as far as 33 deg (angular separation) or 29 kpc from the LMC center.
Our detections reinforce the idea that the halo of the LMC seems to be larger
than previously expected, and its debris can be spread in the sky out to very
large separations from the LMC center. Finally, we provide some kinematic
evidence that many of the stars analysed here have likely come from the Small
Magellanic Cloud.Comment: 15 pages, 13 figures, accepted for publication in MNRA
Spectroscopy of QUEST RR Lyrae Variables: the new Virgo Stellar Stream
Eighteen RR Lyrae variables (RRLs) that lie in the "12\fh 4 clump"
identified by the QUEST survey have been observed spectroscopically to measure
their radial velocities and metal abundances. Ten blue horizontal branch (BHB)
stars identified by the Sloan Digital Sky Survey (SDSS) were added to this
sample. Six of the 9 stars in the densest region of the clump have a mean
radial velocity in the galactic rest frame () of 99.8 and
= 17.3 , which is slightly smaller than the average error of
the measurements. The whole sample contains 8 RRLs and 5 BHB stars that have
values of suggesting membership in this stream. For 7 of these
RRLs, the measurements of [Fe/H], which have an internal precision of 0.08 dex,
yield and = 0.40. These values suggest that
the stream is a tidally disrupted dwarf spheroidal galaxy of low luminosity.
Photometry from the database of the SDSS indicates that this stream covers at
least 106 deg of the sky in the constellation Virgo. The name Virgo Stellar
Stream is suggested.Comment: Replaced with revised version accepted for publication in ApJ Letters
13 pages 4 figure
New Optical Reddening Maps of the Large and Small Magellanic Clouds
We present new reddening maps of the SMC and LMC based on the data of the
third phase of the Optical Gravitational Lensing Experiment (OGLE III). We have
used two different methods to derive optical reddening maps. We adopt a
theoretical mean unreddened colour for the red clump in the SMC and LMC,
respectively. We subdivide the photometric data for both Clouds into subfields
and calculate the difference between the observed red clump position and the
theoretical value for each field, which provides us with the reddening value in
(V-I). Furthermore reddening values are obtained for 13490 LMC RR Lyrae ab and
1529 SMC RR Lyrae ab stars covering the whole OGLE III region of the MCs. The
observed colours (V-I) of the RR Lyrae stars are compared with the colour from
the absolute magnitudes. The absolute magnitude of each RR Lyrae star is
computed using its period and metallicity derived from Fourier decomposition of
its lightcurve. In general we find a low and uniform reddening distribution in
both Magellanic Clouds. The red clump method indicates a mean reddening of the
LMC of E(V-I) = 0.09 +/- 0.07 mag, while for the SMC E(V-I) = 0.04 +/- 0.06 mag
is obtained. With RR Lyrae stars a median value of E(V-I) = 0.11 +/- 0.06 mag
for the LMC and E(V-I) = 0.07 +/- 0.06 mag for the SMC is found. The LMC shows
very low reddening in the bar region, whereas the reddening in the star-forming
leading edge and 30 Doradus is considerably higher. In the SMC three pronounced
regions with higher reddening are visible. Two are located along the bar, while
the highest reddening is found in the star-forming wing of the SMC. In general
the regions with higher reddening are in good spatial agreement with infrared
reddening maps as well as with reddening estimations of other studies. The
position-dependent reddening values from the red clump method are available via
the Virtual Observatory interface.Comment: 15 pages, 22 Figures, AJ publishe
Metallicity distribution functions of the old populations of the Magellanic Clouds from RR Lyrae stars
We present the first metallicity distribution functions of the old field
populations in the Magellanic Clouds. Our metallicities are based on the
Fourier decomposition of Type ab RR Lyrae light curves from the Optical
Gravitational Lensing Experiment (OGLE-III). On the metallicity scale of Zinn &
West; we find a mean metallicity of [Fe/H] = -1.50 +/- 0.24 dex based on 16776
RR Lyrae stars in the Large Magellanic Cloud (LMC). For the Small Magellanic
Cloud (SMC) we obtain -1.70 +/- 0.27 dex based on 1831 RR Lyrae stars. These
uncertainties represent the intrinsic spread in the population rather than the
standard deviation of the mean. Our results are in good agreement with the few
existing spectroscopic metallicity determinations for LMC RR Lyrae stars from
the literature. For both the LMC and the SMC the metallicity spread exceeds 1
dex in [Fe/H]. The distribution of metallicities in both Clouds is very
uniform, and no significant metallicity gradient is detectable. We also do not
find any pronounced populations of extremely metal-poor RR Lyrae candidates
with metallicities well below -2 dex, although we need to caution that the
photometric method used may overestimate the metallicities of metal-deficient
stars. Moreover, because of stellar evolutionary effects one does not expect to
observe many RR Lyrae stars among very metal-poor horizontal branch stars. We
suggest that the Magellanic Clouds experienced fairly rapid and efficient early
enrichment involving pre-enriched gas as well as possibly gas infall, while
metal loss through outflows does not seem to have played a significant role.
Moreover we suggest that the differences in the metallicities of the old
population of LMC and SMC make an origin from a single, common progenitor
unlikely, unless the separation happened very early on.Comment: Accepted for publication in AJ, 12 pages, 13 figure