Bandwidth in bolometric interferometry

Charlassier, R.; Bunn, Emory F.; Hamilton, J. C.; Kaplan, J.; Malu, Siddharth

doi:10.1051/0004-6361/200913446

Cited by 6 publications

(4 citation statements)

References 10 publications

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“…The interferometric part of the model requires the computation of the Thiele-Innes (geometrical) coefficients to determine the position angle and separation of the system (Hilditch 2001). The smearing of the V 2 induced by the IOTA-IONIC bandwidth of 0.3μm is accounted for (Zhao et al 2007;Charlassier et al 2010). The code includes the array configuration and target coordinates for each epoch.…”

Section: Orbit Analysismentioning

confidence: 99%

A Precise Physical Orbit for the M-Dwarf Binary Gliese 268

Barry

Demory

Ségransan

et al. 2012

ApJ

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We report high-precision interferometric and radial velocity (RV) observations of the M-dwarf binary Gl 268. Combining measurements conducted using the IOTA interferometer and the ELODIE and Harvard Center for Astrophysics RV instruments leads to a mass of 0.22596 ± 0.00084 M for component A and 0.19230 ± 0.00071 M for component B. The system parallax as determined by these observations is 0.1560 ± 0.0030 arcsec-a measurement with 1.9% uncertainty in excellent agreement with Hipparcos (0.1572 ± 0.0033). The absolute H-band magnitudes of the component stars are not well constrained by these measurements; however, we can place an approximate upper limit of 7.95 and 8.1 for Gl 268A and B, respectively. We test these physical parameters against the predictions of theoretical models that combine stellar evolution with high fidelity, non-gray atmospheric models. Measured and predicted values are compatible within 2σ. These results are among the most precise masses measured for visual binaries and compete with the best adaptive optics and eclipsing binary results.

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Section: Orbit Analysismentioning

confidence: 99%

A Precise Physical Orbit for the M-Dwarf Binary Gliese 268

Barry

Demory

Ségransan

et al. 2012

ApJ

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“…Application to CMB cosmology: The QUBIC collaboration is implementing the technique described in this paper (Charlassier et al 2010).…”

Section: Effect Of Finite Detector Sizementioning

confidence: 99%

Broadband Fizeau Interferometers for Astrophysics

Malu,

Timbie

2010

Preprint

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Context. Measurements of the 2.7 K cosmic microwave background (CMB) radiation now provide the most stringent constraints on cosmological models. The power spectra of the temperature anisotropies and the E-mode polarization of the CMB are explained well by the inflationary paradigm. The next generation of CMB experiments aim at providing the most direct evidence for inflation through the detection of B-modes in the CMB polarization, presumed to have been caused by gravitational waves generated during the inflationary epoch around 10 −34 s. The B-mode polarization signals are very small (≤10 −8 K) compared with the temperature anisotropies (∼ 10 −4 K). Systematic effects in CMB telescopes can cause leakage from temperature anisotropy into polarization. Bolometric interferometry (BI) is a novel approach to measuring this small signal with lower leakage. Aims. If BI can be made to work over wide bandwidth (∼ 20 − 30%) it can provide similar sensitivity to imagers. Subdividing the frequency passband of a Fizeau interferometer would mitigate the problem of 'fringe smearing.' Furthermore, the approach should allow simultaneous measurements in image space and visibility space. Methods. For subdividing the frequency passsband ('sub-band splitting' henceforth), we write an expression for the output from every baseline at every detector in the focal plane as a sum of visibilities in different frequency sub-bands. For operating the interferometer simultaneously as an imager, we write the output as two integrals over the sky and the focal plane, with all the phase differences accounted for. Results. The sub-band splitting method described here is general and can be applied to broad-band Fizeau interferometers across the electromagnetic spectrum. Applications to CMB measurements and to long-baseline optical interferometry are promising.

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“…There may well be other data analysis methods that do not involve worrying about an E/B/A decomposition. For example, one might analyze interferometric data entirely in visibility space [30][31][32], without ever constructing a real-space map at all.…”

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confidence: 99%

Efficient decomposition of cosmic microwave background polarization maps into pureE, pureB, and ambiguous components

Bunn

2011

Phys. Rev. D

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Separation of the B component of a cosmic microwave background (CMB) polarization map from the much larger E component is an essential step in CMB polarimetry. For a map with incomplete sky coverage, this separation is necessarily hampered by the presence of "ambiguous" modes which could be either E or B modes. I present an efficient pixel-space algorithm for removing the ambiguous modes and separating the map into "pure" E and B components. The method, which works for arbitrary geometries, does not involve generating a complete basis of such modes and scales the cube of the number of pixels on the boundary of the map.

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Bandwidth in bolometric interferometry

Cited by 6 publications

References 10 publications

A Precise Physical Orbit for the M-Dwarf Binary Gliese 268

A Precise Physical Orbit for the M-Dwarf Binary Gliese 268

Broadband Fizeau Interferometers for Astrophysics

Efficient decomposition of cosmic microwave background polarization maps into pureE, pureB, and ambiguous components

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