-
M J Kim,
S Kim,
S. Youn,
M. S. Yun,
G W Wilson,
I. Aretxaga,
J. P. Williams,
D. H. Hughes,
A. Humphrey,
J. E. Austermann,
T. A. Perera, P. D. Mauskopf,
L. Magnani,
Y. -W. Kang
[show abstract]
[hide abstract]
ABSTRACT: We present 1.1 mm observations of the dust continuum emission from the MBM12
high-latitude molecular cloud observed with the Astronomical Thermal Emission
Camera (AzTEC) mounted on the James Clerk Maxwell Telescope on Mauna Kea,
Hawaii. We surveyed a 6.34 deg$^2$ centered on MBM12, making this the largest
area that has ever been surveyed in this region with submillimeter and
millimeter telescopes. Eight secure individual sources were detected with a
signal-to-noise ratio of over 4.4. These eight AzTEC sources can be considered
to be real astronomical objects compared to the other candidates based on
calculations of the false detection rate. The distribution of the detected 1.1
mm sources or compact 1.1 mm peaks is spatially anti-correlated with that of
the 100 micronm emission and the $^{12}$CO emission. We detected the 1.1 mm
dust continuum emitting sources associated with two classical T Tauri stars,
LkHalpha262 and LkHalpha264. Observations of spectral energy distributions
(SEDs) indicate that LkHalpha262 is likely to be Class II (pre-main-sequence
star), but there are also indications that it could be a late Class I
(protostar). A flared disk and a bipolar cavity in the models of Class I
sources lead to more complicated SEDs. From the present AzTEC observations of
the MBM12 region, it appears that other sources detected with AzTEC are likely
to be extragalactic and located behind MBM12. Some of these have radio
counterparts and their star formation rates are derived from a fit of the SEDs
to the photometric evolution of galaxies in which the effects of a dusty
interstellar medium have been included.
12/2011;
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S. Ikarashi,
K. Kohno,
J. E. Aguirre,
I. Aretxaga,
V. Arumugam,
J. E. Austermann,
J. J. Bock,
C. M. Bradford,
M. Cirasuolo,
L. Earle, [......],
K. Shimasaku,
T. Takagi,
T. Takata,
Y. Tamura,
K. Tanaka,
T. Tsukagoshi,
D. J. Wilner,
G. W. Wilson,
M. S. Yun,
J. Zmuidzinas
[show abstract]
[hide abstract]
ABSTRACT: We report on the detection of an extremely bright (∼37 mJy at 1100 μm and ∼91 mJy at 880 μm) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in the 1100 μm observations of the Subaru/XMM–Newton Deep Field using AzTEC on ASTE. Subsequent CARMA 1300-μm and SMA 880-μm observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended [full width at half-maximum (FWHM) of ∼4 arcsec] and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide-band spectrum from 190 to 308 GHz, although no significant emission/absorption lines were found. The derived upper limit to the line-to-continuum flux ratio is 0.1–0.3 (2σ) across the Z-Spec band.Based on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at z ∼ 3.4 behind a foreground, optically visible (but red) galaxy at z ∼ 1.4. The deduced apparent (i.e., no correction for magnification) infrared luminosity (LIR) and star formation rate (SFR) are 6 × 1013 L⊙ and 11 000 M⊙ yr−1, respectively, assuming that the LIR is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time-scale (3 × 107 yr), which is indeed comparable to those in extreme starbursts like the centres of local ultraluminous infrared galaxies (ULIRGs).
Monthly Notices of the Royal Astronomical Society 08/2011; 415(4):3081 - 3096. · 4.90 Impact Factor
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S. Ikarashi,
K Kohno,
J. E. Aguirre,
I. Aretxaga,
V. Arumugam,
J. E. Austermann,
J. J. Bock,
C. M. Bradford,
M. Cirasuolo,
L. Earle, [......],
K. Shimasaku,
T Takagi,
T Takata,
Y Tamura,
K Tanaka,
T. Tsukagoshi,
D. J. Wilner,
G W Wilson,
M. S. Yun,
J. Zmuidzinas
[show abstract]
[hide abstract]
ABSTRACT: We report the detection of an extremely bright ($\sim$37 mJy at 1100 $\mu$m
and $\sim$91 mJy at 880 $\mu$m) submillimeter galaxy (SMG),
AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi),
discovered in 1100 $\mu$m observations of the Subaru/XMM-Newton Deep Field
using AzTEC on ASTE. Subsequent CARMA 1300 $\mu$m and SMA 880 $\mu$m
observations successfully pinpoint the location of Orochi and suggest that it
has two components, one extended (FWHM of $\sim$ 4$^{\prime\prime}$) and one
compact (unresolved). Z-Spec on CSO has also been used to obtain a wide band
spectrum from 190 to 308 GHz, although no significant emission/absorption lines
are found. The derived upper limit to the line-to-continuum flux ratio is
0.1--0.3 (2 $\sigma$) across the Z-Spec band.
Based on the analysis of the derived spectral energy distribution from
optical to radio wavelengths of possible counterparts near the SMA/CARMA peak
position, we suggest that Orochi is a lensed, optically dark SMG lying at $z
\sim 3.4$ behind a foreground, optically visible (but red) galaxy at $z \sim
1.4$. The deduced apparent (i.e., no correction for magnification) infrared
luminosity ($L_{\rm IR}$) and star formation rate (SFR) are $6 \times 10^{13}$
$L_{\odot}$ and 11000 $M_{\odot}$ yr$^{-1}$, respectively, assuming that the
$L_{\rm IR}$ is dominated by star formation. These values suggest that Orochi
will consume its gas reservoir within a short time scale ($3 \times 10^{7}$
yr), which is indeed comparable to those in extreme starbursts like the centres
of local ULIRGs.
09/2010;
-
[show abstract]
[hide abstract]
ABSTRACT: We present an analysis of an 8 arcminute diameter map of the area around the galaxy cluster Abell 1835 from jiggle map observations at a wavelength of 1.1 mm using the Bolometric Camera (Bolocam) mounted on the Caltech Submillimeter Observa-tory (CSO). The data is well described by a model including an extended Sunyaev-Zel'dovich (SZ) signal from the cluster gas plus emission from two bright background submm galaxies magnified by the gravitational lensing of the cluster. The best-fit values for the central Compton value for the cluster and the fluxes of the two main point sources in the field: SMM J140104+0252, and SMM J14009+0252 are found to be y 0 = (4.34 ± 0.52 ± 0.69) × 10 −4 , 6.5±2.0 ± 0.7 mJy and 11.3±1.9 ± 1.1 mJy, where the first error represents the statistical measurement error and the second error represents the estimated systematic error in the result. This measurement assumes the presence of dust emission from the cluster's central cD galaxy of 1.8 ± 0.5 mJy, based on higher frequency observations of Abell 1835. The cluster image represents one of the highest-significance SZ detections of a cluster in the positive region of the thermal SZ spectrum to date. The inferred central intensity is compared to other SZ measurements of Abell 1835 and this collection of results is used to obtain values for y 0 = (3.60 ± 0.24) × 10 −4 and the cluster peculiar velocity v z = −226 ± 275 km/s.
Mon. Not. R. Astron. Soc. 04/2010; 000:1-10.
-
M. Veneziani,
P. A. R. Ade,
J. J. Bock,
A. Boscaleri,
B. P. Crill,
P. de Bernardis,
G. De Gasperis,
A. de Oliveira-Costa,
G. De Troia,
G. Di Stefano, [......],
T. E. Montroy,
P. Natoli,
C. B. Netterfield,
E. Pascale,
F. Piacentini,
D. Pietrobon,
G. Polenta,
S. Ricciardi,
G. Romeo,
and J. E. Ruhl
[show abstract]
[hide abstract]
ABSTRACT: The physical properties of galactic cirrus emission are not well characterized. BOOMERANG is a balloon-borne experiment designed to study the cosmic microwave background at high angular resolution in the millimeter range. The BOOMERANG 245 and 345 GHz channels are sensitive to interstellar signals, in a spectral range intermediate between FIR and microwave frequencies. We look for physical characteristics of cirrus structures in a region at high galactic latitudes (b ~ –40°) where BOOMERANG performed its deepest integration, combining the BOOMERANG data with other available data sets at different wavelengths. We have detected eight emission patches in the 345 GHz map, consistent with cirrus dust in the Infrared Astronomical Satellite maps. The analysis technique we have developed allows us to identify the location and the shape of cirrus clouds, and to extract the flux from observations with different instruments at different wavelengths and angular resolutions. We study the integrated flux emitted from these cirrus clouds using data from Infrared Astronomical Satellite (IRAS), DIRBE, BOOMERANG and Wilkinson Microwave Anisotropy Probe in the frequency range 23-3000 GHz (13 mm-100 μm wavelength). We fit the measured spectral energy distributions with a combination of a gray body and a power-law spectra considering two models for the thermal emission. The temperature of the thermal dust component varies in the 7-20 K range and its emissivity spectral index is in the 1-5 range. We identified a physical relation between temperature and spectral index as had been proposed in previous works. This technique can be proficiently used for the forthcoming Planck and Herschel missions data.
The Astrophysical Journal 03/2010; 713(2):959. · 6.02 Impact Factor
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K. S. Scott,
M. S. Yun,
G W Wilson,
J. E. Austermann,
E. Aguilar,
I. Aretxaga,
H. Ezawa,
D. Ferrusca,
B. Hatsukade,
D. H. Hughes, [......],
K Kohno, P. D. Mauskopf,
T Oshima,
T. A. Perera,
J. Rand,
Y Tamura,
T. Tosaki,
M. Velazquez,
C. C. Williams,
M. Zeballos
[show abstract]
[hide abstract]
ABSTRACT: [Abridged] We present the first results from a 1.1 mm confusion-limited map of the GOODS-S field taken with AzTEC on the ASTE telescope. We imaged a 270 sq. arcmin field to a 1\sigma depth of 0.48 - 0.73 mJy/beam, making this one of the deepest blank-field surveys at mm-wavelengths ever achieved. Although our GOODS-S map is extremely confused, we demonstrate that our source identification and number counts analyses are robust, and the techniques discussed in this paper are relevant for other deeply confused surveys. We find a total of 41 dusty starburst galaxies with S/N >= 3.5 within this uniformly covered region, where only two are expected to be false detections. We derive the 1.1mm number counts from this field using both a "P(d)" analysis and a semi-Bayesian technique, and find that both methods give consistent results. Our data are well-fit by a Schechter function model with (S', N(3mJy), \alpha) = (1.30+0.19 mJy, 160+27 (mJy/deg^2)^(-1), -2.0). Given the depth of this survey, we put the first tight constraints on the 1.1 mm number counts at S(1.1mm) = 0.5 mJy, and we find evidence that the faint-end of the number counts at S(850\mu m) < 2.0 mJy from various SCUBA surveys towards lensing clusters are biased high. In contrast to the 870 \mu m survey of this field with the LABOCA camera, we find no apparent under-density of sources compared to previous surveys at 1.1 mm. Additionally, we find a significant number of SMGs not identified in the LABOCA catalogue. We find that in contrast to observations at wavelengths < 500 \mu m, MIPS 24 \mu m sources do not resolve the total energy density in the cosmic infrared background at 1.1 mm, demonstrating that a population of z > 3 dust-obscured galaxies that are unaccounted for at these shorter wavelengths potentially contribute to a large fraction (~2/3) of the infrared background at 1.1 mm. Comment: 21 pages, 9 figures. Accepted to MNRAS
03/2010;
-
J. Sayers,
S. R. Golwala,
P. A. R. Ade,
J. E. Aguirre,
J. J. Bock,
S. F. Edgington,
J. Glenn,
A. Goldin,
D. Haig,
A. E. Lange,
G. T. Laurent, P. D. Mauskopf,
H. T. Nguyen,
P. Rossinot,
and J. Schlaerth
[show abstract]
[hide abstract]
ABSTRACT: We report measurements of the fluctuations in atmospheric emission (atmospheric noise) above Mauna Kea recorded with Bolocam at 143 and 268 GHz from the Caltech Submillimeter Observatory. The 143 GHz data were collected during a 40 night observing run in late 2003, and the 268 GHz observations were made in early 2004 and early 2005 over a total of 60 nights. Below 0.5 Hz, the data time-streams are dominated by atmospheric noise in all observing conditions. The atmospheric noise data are consistent with a Kolmogorov-Taylor turbulence model for a thin wind-driven screen, and the median amplitude of the fluctuations is 280 mK2 rad–5/3 at 143 GHz and 4000 mK2 rad–5/3 at 268 GHz. Comparing our results with previous ACBAR data, we find that the normalization of the power spectrum of the atmospheric noise fluctuations is a factor of 80 larger above Mauna Kea than above the South Pole at millimeter wavelengths. Most of this difference is due to the fact that the atmosphere above the South Pole is much drier than the atmosphere above Mauna Kea. However, the atmosphere above the South Pole is slightly more stable as well: the fractional fluctuations in the column depth of precipitable water vapor are a factor of smaller at the South Pole compared to Mauna Kea. Based on our atmospheric modeling, we developed several algorithms to remove the atmospheric noise, and the best results were achieved when we described the fluctuations using a low-order polynomial in detector position over the 8' field of view. However, even with these algorithms, we were not able to reach photon-background-limited instrument photometer performance at frequencies below 0.5 Hz in any observing conditions. We also observed an excess low-frequency noise that is highly correlated between detectors separated by (f/#)λ; this noise appears to be caused by atmospheric fluctuations, but we do not have an adequate model to explain its source. We hypothesize that the correlations arise from the classical coherence of the electromagnetic field across a distance of (f/#)λ on the focal plane.
The Astrophysical Journal 12/2009; 708(2):1674. · 6.02 Impact Factor
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J. L. Wardlow,
Ian Smail,
G W Wilson,
M. S. Yun,
K. E. K. Coppin,
R. Cybulski,
J. E. Geach,
R. J. Ivison,
I. Aretxaga,
J. E. Austermann,
A. C. Edge,
G. G. Fazio,
J Huang,
D. H. Hughes,
T Kodama,
Y. Kang,
S Kim, P. D. Mauskopf,
T. A. Perera,
K. S. Scott
[show abstract]
[hide abstract]
ABSTRACT: We have undertaken a deep (sigma~1.1 mJy) 1.1-mm survey of the z=0.54 cluster MS 0451.6-0305 using the AzTEC camera on the James Clerk Maxwell Telescope. We detect 36 sources with S/N>3.5 in the central 0.10 deg^2 and present the AzTEC map, catalogue and number counts. We identify counterparts to 18 sources (50%) using radio, mid-infrared, Spitzer IRAC and Submillimeter Array data. Optical, near- and mid-infrared spectral energy distributions are compiled for the 14 of these galaxies with detectable counterparts, which are expected to contain all likely cluster members. We then use photometric redshifts and colour selection to separate background galaxies from potential cluster members and test the reliability of this technique using archival observations of submillimetre galaxies. We find two potential MS 0451-03 members, which, if they are both cluster galaxies have a total star-formation rate (SFR) of ~100 solar masses per year -- a significant fraction of the combined SFR of all the other galaxies in MS 0451-03. We also examine the stacked rest-frame mid-infrared, millimetre and radio emission of cluster members below our AzTEC detection limit and find that the SFRs of mid-IR selected galaxies in the cluster and redshift-matched field populations are comparable. In contrast, the average SFR of the morphologically classified late-type cluster population is ~3 times less than the corresponding redshift-matched field galaxies. This suggests that these galaxies may be in the process of being transformed on the red-sequence by the cluster environment. Our survey demonstrates that although the environment of MS 0451-03 appears to suppress star-formation in late-type galaxies, it can support active, dust-obscured mid-IR galaxies and potentially millimetre-detected LIRGs. Comment: 20 pages, 9 figures, 5 tables. Accepted for publication in MNRAS. High resolution version available at http://www.astro.dur.ac.uk/~d30qst/papers/aztec_ms0451.pdf
10/2009;
-
M. Veneziani,
A. Amblard,
A. Cooray,
F. Piacentini,
D. Pietrobon,
P. Serra,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill, [......],
P. Natoli,
C. B. Netterfield,
E. Pascale,
G. Polenta,
S. Ricciardi,
G. Romeo,
J. E. Ruhl,
P. Santini,
M. Tegmark,
and N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: The Sunyaev-Zel'dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB data sets. Using CMB anisotropies measured at three frequencies by the BOOMERANG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 μK (2σ) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERANG SZ data alone is σSZ 8 < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find σSZ 8 < 0.92 (95% c.l.).
The Astrophysical Journal 08/2009; 702(1):L61. · 6.02 Impact Factor
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J. E. Austermann,
J. S. Dunlop,
T. A. Perera,
K. S. Scott,
G W Wilson,
I. Aretxaga,
D. H. Hughes,
O. Almaini,
E. L. Chapin,
S. C. Chapman, [......],
I. Roseboom,
M. Rowan-Robinson,
D Scott,
S. Serjeant,
I. Smail,
A. M. Swinbank,
J. A. Stevens,
M. Velazquez,
J. Wagg,
M. S. Yun
[show abstract]
[hide abstract]
ABSTRACT: We present the first results from the largest deep extragalactic millimetre-wavelength survey undertaken to date. These results are derived from maps covering over 0.7 deg^2, made at 1.1mm, using the AzTEC continuum camera mounted on the James Clerk Maxwell Telescope. The maps were made in the two fields originally targeted at 0.85mm with SCUBA in the SHADES project, namely the Lockman Hole East (mapped to a depth of 0.9-1.3 mJy rms) and the Subaru XMM Deep Field (1.0-1.7 mJy rms). The wealth of existing and forthcoming deep multi-frequency data in these two fields will allow the bright mm source population revealed by these images to be explored in detail in subsequent papers. Here we present the maps themselves, a catalogue of 114 high-significance sub-millimetre galaxy detections, and a thorough statistical analysis leading to the most robust determination to date of the 1.1mm source number counts. Through careful comparison, we find that both the COSMOS and GOODS North fields, also imaged with AzTEC, contain an excess of mm sources over the new 1.1mm source-count baseline established here. In particular, our new AzTEC/SHADES results indicate that very luminous high-redshift dust enshrouded starbursts (S_{1.1} > 3 mJy) are 25-50% less common than would have been inferred from these smaller surveys, thus highlighting the potential roles of cosmic variance and clustering in such measurements. We compare number count predictions from recent models of the evolving mm/sub-mm source population to these SMG surveys, which provide important constraints for the ongoing refinement of semi-analytic and hydrodynamical models of galaxy formation, and find that all recent models over-predict the number of bright sub-millimetre galaxies found in this survey. Comment: 19 pages, 10 figures, 7 tables - Very minor revisions; accepted for publication in MNRAS
07/2009;
-
P. Natoli,
G. De Troia,
C. Hikage,
E. Komatsu,
M. Migliaccio,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri, [......],
C. B. Netterfield,
E. Pascale,
F. Piacentini,
G. Polenta,
S Ricciardi,
G Romeo,
J. E. Ruhl,
M. Tegmark,
M. Veneziani,
N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: We use Minkowski Functionals (MF) to constrain a primordial non-Gaussian contribution to the CMB intensity field as observed in the 150 GHz and 145 GHz BOOMERanG maps from the 1998 and 2003 flights, respectively, performing for the first time a joint analysis of the two datasets. A perturbative expansion of the MF formulae in the limit of a weakly non-Gaussian field yields analytical formulae, derived by Hikage et al. (2006), which can be used to constrain the coupling parameter f_NL without the need for non-Gaussian simulations. We find -1020<f_NL<390 at 95% CL, significantly improving the previous constraints by De Troia et al. (2007) on the BOOMERanG 2003 dataset. These are the best f_NL limits to date for suborbital probes. Comment: 8 pages, 3 figures
05/2009;
-
J. Sayers,
S. R. Golwala,
P. Rossinot,
P. A. R. Ade,
J. E. Aguirre,
J. J. Bock,
S. F. Edgington,
J. Glenn,
A. Goldin,
D. Haig,
A. E. Lange,
G. T. Laurent, P. D. Mauskopf,
and H. T. Nguyen
[show abstract]
[hide abstract]
ABSTRACT: We have surveyed two science fields totaling 1 deg2 with Bolocam at 2.1 mm to search for secondary Cosmic Microwave Background (CMB) anisotropies caused by the Sunyaev-Zel'dovich effect (SZE). The fields are in the Lynx and Subaru/XMM SDS1 fields. Our survey is sensitive to angular scales with an effective angular multipole of ℓeff = 5700 with FWHMℓ = 2800 and has an angular resolution of 60 arcsec FWHM. Our data provide no evidence for anisotropy. We are able to constrain the level of total astronomical anisotropy, modeled as a flat-band power in , with most frequent 68%, 90%, and 95% CL upper limits of 590, 760, and 830 μK 2 CMB. We statistically subtract the known contribution from primary CMB anisotropy, including cosmic variance, to obtain constraints on the SZE anisotropy contribution. Now including flux calibration uncertainty, our most frequent 68%, 90%, and 95% CL upper limits on a flat-band power in are 690, 960, and 1000 μK 2 CMB. When we instead employ the analytical spectrum suggested by Komatsu and Seljack in 2002, and account for the non-Gaussianity of the SZE anisotropy signal, we obtain upper limits on the average amplitude of their spectrum weighted by our transfer function of 790, 1060, and 1080 μK 2 CMB. We obtain a 90% CL upper limit on σ8, which normalizes the power spectrum of density fluctuations, of 1.57. These are the first constraints on anisotropy and σ8 from survey data at these angular scales at frequencies near 150 GHz.
The Astrophysical Journal 12/2008; 690(2):1597. · 6.02 Impact Factor
-
C. J. MacTavish,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri,
P. Cabella,
C. R. Contaldi,
B. P. Crill,
P. de Bernardis, [......],
D. Pogosyan,
G. Polenta,
S. Prunet,
S. Ricciardi,
G. Romeo,
J. E. Ruhl,
P. Santini,
M. Tegmark,
M. Veneziani,
and N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: We present the cosmological parameters from the CMB intensity and polarization power spectra of the 2003 Antarctic flight of the BOOMERANG telescope. The BOOMERANG data alone constrain the parameters of the ΛCDM model remarkably well and are consistent with constraints from a multiexperiment combined CMB data set. We add LSS data from the 2dF and SDSS redshift surveys to the combined CMB data set and test several extensions to the standard model including running of the spectral index, curvature, tensor modes, the effect of massive neutrinos, and an effective equation of state for dark energy. We also include an analysis of constraints to a model that allows a CDM isocurvature admixture.
The Astrophysical Journal 12/2008; 647(2):799. · 6.02 Impact Factor
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F. Piacentini,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri,
P. Cabella,
C. R. Contaldi,
B. P. Crill,
P. de Bernardis, [......],
D. Pogosyan,
G. Polenta,
S. Prunet,
S. Ricciardi,
G. Romeo,
J. E. Ruhl,
P. Santini,
M. Tegmark,
M. Veneziani,
and N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: We present a measurement of the polarization-temperature angular cross power spectra, TE and TB, of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant TE correlation in the l-range between 50 and 950 with a statistical significance of >3.5 σ. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the "concordance model" that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.
The Astrophysical Journal 12/2008; 647(2):833. · 6.02 Impact Factor
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A. Melchiorri,
P. A. R. Ade,
P. de Bernardis,
J. J. Bock,
J. Borrill,
A. Boscaleri,
B. P. Crill,
G. De Troia,
P. Farese,
P. G. Ferreira, [......],
A. E. Lange,
S. Masi, P. D. Mauskopf,
L. Miglio,
C. B. Netterfield,
E. Pascale,
F. Piacentini,
G. Romeo,
J. E. Ruhl,
and N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: We use the angular power spectrum of the cosmic microwave background, measured during the North American test flight of the Boomerang experiment, to constrain the geometry of the universe. Within the class of cold dark matter models, we find that the overall fractional energy density of the universe Ω is constrained to be 0.85 ≤ Ω ≤ 1.25 at the 68% confidence level. Combined with the COBE measurement, the data on degree scales from the Microwave Anisotropy Telescope in Chile, and the high-redshift supernovae data, we obtain new constraints on the fractional matter density and the cosmological constant.
The Astrophysical Journal 12/2008; 536(2):L63. · 6.02 Impact Factor
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P. de Bernardis,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri,
K. Coble,
C. R. Contaldi,
B. P. Crill,
G. De Troia, [......],
C. B. Netterfield,
E. Pascale,
F. Piacentini,
D. Pogosyan,
G. Polenta,
F. Pongetti,
S. Prunet,
G. Romeo,
J. E. Ruhl,
and F. Scaramuzzi
[show abstract]
[hide abstract]
ABSTRACT: Three peaks and two dips have been detected in the power spectrum of the cosmic microwave background by the BOOMERANG experiment, at l = (213), (541), (845) and l = (416), (750), respectively. Using model-independent analyses, we find that all five features are statistically significant, and we measure their location and amplitude. These are consistent with the adiabatic inflationary model. We also calculate the mean and variance of the peak and dip locations and amplitudes in a large seven-dimensional parameter space of such models, which gives good agreement with the model-independent estimates. We forecast where the next few peaks and dips should be found if the basic paradigm is correct. We test the robustness of our results by comparing Bayesian marginalization techniques on this space with likelihood maximization techniques applied to a second seven-dimensional cosmological parameter space, using an independent computational pipeline, and find excellent agreement: Ωtot = 1.02 versus 1.04 ± 0.05, Ωbh2 = 0.022 versus 0.019, and ns = 0.96 versus 0.90 ± 0.08. The determination of the best fit by the maximization procedure effectively ignores nonzero optical depth of reionization τC > 0, and the difference in primordial spectral index ns between the two methods is thus a consequence of the strong correlation of ns with the τC.
The Astrophysical Journal 12/2008; 564(2):559. · 6.02 Impact Factor
-
G. Polenta,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri,
C. R. Contaldi,
B. P. Crill,
P. de Bernardis,
G. De Gasperis, [......],
P. Natoli,
C. B. Netterfield,
E. Pascale,
F. Piacentini,
D. Pogosyan,
S. Prunet,
G. Romeo,
J. E. Ruhl,
N. Vittorio,
and A. Zeppilli
[show abstract]
[hide abstract]
ABSTRACT: We search the BOOMERANG (Balloon Observations Of Millimetric Extragalactic Radiation ANd Geophysics) maps of the anisotropy of the cosmic microwave background (CMB) for deviations from Gaussianity. In this Letter, we focus on analysis techniques in pixel space and compute skewness, kurtosis, and Minkowski functionals for the BOOMERANG maps and for Gaussian simulations of the CMB sky. We do not find any significant deviation from Gaussianity in the high galactic latitude section of the 150 GHz map. We do find deviations from Gaussianity at lower latitudes and at 410 GHz, and we ascribe them to Galactic dust contamination. Using non-Gaussian simulations of instrumental systematic effects, of foregrounds, and of sample non-Gaussian cosmological models, we set upper limits to the non-Gaussian component of the temperature field in the BOOMERANG maps. For fluctuations distributed as a 1 degree of freedom χ2 mixed to the main Gaussian component, our upper limits are in the few percentile range.
The Astrophysical Journal 12/2008; 572(1):L27. · 6.02 Impact Factor
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S. Masi,
P. A. R. Ade,
J. J. Bock,
A. Boscaleri,
B. P. Crill,
P. de Bernardis,
M. Giacometti,
E. Hivon,
V. V. Hristov,
A. E. Lange, P. D. Mauskopf,
T. Montroy,
C. B. Netterfield,
E. Pascale,
F. Piacentini,
S. Prunet,
and J. Ruhl
[show abstract]
[hide abstract]
ABSTRACT: We present millimeter-wave observations obtained by the BOOMERANG (Balloon Observations Of Millimetric Extragalactic Radiation ANd Geophysics) experiment of Galactic emission at intermediate and high (b < -20°) Galactic latitudes. We find that this emission is well correlated with extrapolated dust maps and is spectrally consistent with thermal emission from interstellar dust (ISD). The ISD brightness in the 410 GHz map has an angular power spectrum cl ~ l-β with 2 β 3. At 150 GHz and at multipoles l ~ 200, the angular power spectrum of the IRAS-correlated dust signal is estimated to be l(l + 1)cl/2π = 3.7 ± 2.9 μK2. This is negligible with respect to the cosmic microwave background (CMB) signal measured by the same experiment l(l + 1)cl/2π = 4700 ± 540 μK2. For the uncorrelated dust signal, we set an upper limit to the contribution to the CMB power at 150 GHz and l ~ 200 of l(l + 1)cl/2π < 3 μK 2 at 95% CL.
The Astrophysical Journal 12/2008; 553(2):L93. · 6.02 Impact Factor
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F. Piacentini,
P. A. R. Ade,
R. S. Bhatia,
J. J. Bock,
A. Boscaleri,
P. Cardoni,
B. P. Crill,
P. de Bernardis,
H. Del Castillo,
G. De Troia, [......], P. D. Mauskopf,
L. Miglio,
C. B. Netterfield,
P. Palangio,
E. Pascale,
A. Raccanelli,
S. Rao,
G. Romeo,
J. Ruhl,
and F. Scaramuzzi
[show abstract]
[hide abstract]
ABSTRACT: We describe the BOOMERANG North America instrument, a balloon-borne bolometric radiometer designed to map the cosmic microwave background (CMB) radiation with 03 resolution over a significant portion of the sky. This receiver employs new technologies in bolometers, readout electronics, millimeter-wave optics and filters, cryogenics, scan, and attitude reconstruction. All these subsystems are described in detail in this paper. The system has been fully calibrated in flight using a variety of techniques, which are described and compared. Using this system, we have obtained a measurement of the first peak in the CMB angular power spectrum in a single, few hour long balloon flight. The instrument described here was a prototype of the BOOMERANG Long Duration Balloon experiment.
The Astrophysical Journal Supplement Series 12/2008; 138(2):315. · 13.46 Impact Factor
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G. De Troia,
P. A. R. Ade,
J. J. Bock,
J. R. Bond,
J. Borrill,
A. Boscaleri,
P. Cabella,
C. R. Contaldi,
B. P. Crill,
P. de Bernardis, [......],
D. Pogosyan,
G. Polenta,
S. Prunet,
S. Ricciardi,
G. Romeo,
J. E. Ruhl,
P. Santini,
M. Tegmark,
M. Veneziani,
and N. Vittorio
[show abstract]
[hide abstract]
ABSTRACT: We analyze the BOOMERANG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non-Gaussian, primordial contribution to CMB fluctuations. We perform a pixel-space analysis restricted to a portion of the map chosen in view of high-sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high-quality simulated data, including non-Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERANG data for the nonlinear coupling parameter fNL as -300 < fNL < 650 at 68% CL and -800 < fNL < 1050 at 95% CL.
The Astrophysical Journal 12/2008; 670(2):L73. · 6.02 Impact Factor
