Optical Polarimetry: Methods, Instruments and Calibration Techniques

Berdyugin, A.; Piirola, V.; Poutanen, Juri

doi:10.1007/978-3-030-19715-5_3

Cited by 11 publications

(5 citation statements)

References 43 publications

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“…DIPOL-1 observations require standard calibrations, i.e., bias and dark subtraction, and flat-field correction (Berdyugin et al 2019). Bias and dark exposures are taken at the beginning of each observing night.…”

Section: Data Processing and Reductionmentioning

confidence: 99%

“…This step can be performed with the MaxIm DL software. The Stokes parameters Q and U from each four successive exposures made at 22°.5 intervals of the λ/2 plate are calculated from the intensity ratios (see Berdyugin et al 2019). Then, all the individual Stokes parameters are averaged to derive the final Stokes parameters and, thus, the polarization degree and angle values.…”

Section: Data Processing and Reductionmentioning

confidence: 99%

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Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory

Otero-Santos,

Piirola,

Escudero Pedrosa

et al. 2024

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We report here the performance and first results of the new multiband optical polarimeter DIPOL-1, installed at the Sierra Nevada Observatory 90 cm T90 telescope (SNO, Granada, Spain). DIPOL-1 is equipped with a plane parallel calcite plate and λ/2 retarder for modulating the intensity of two perpendicularly polarized beams, and a high readout speed CMOS camera that allows for fast, time-dense coverage. We characterize the performance of this instrument through a series of tests on zero- and high-polarization standard stars. The instrumental polarization in the Nasmyth focus was well determined, with a very stable contribution of 4.0806% ± 0.0014% in the optical R band. For bright high-polarization standards (m R < 8) we reach precisions <0.02% in polarization degree and 0.°1 in polarization angle for exposures of 2–4 min. The polarization properties of these stars have been constrained, providing more recent results also about possible variability for future studies of some of the most used calibrators. Moreover, we have tested the capability of observing much fainter objects, in particular through blazar observations, where we reach a precision of <0.5%−0.6% and <0.°5 for faint targets (m R ∼ 16.5) with exposures of ∼1 hr. For brighter targets (m R ∼ 14.5−15), we can aim for time-dense observations with errors <0.2%−0.4% and <1°−1.°5 in 5–20 min. We have successfully performed a first campaign with DIPOL-1, detecting significant polarized emission of several blazars, with special attention to the highest ever polarization degree measured from blazar 3C 345 at ∼32%.

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Section: Data Processing and Reductionmentioning

confidence: 99%

Section: Data Processing and Reductionmentioning

confidence: 99%

Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory

Otero-Santos,

Piirola,

Escudero Pedrosa

et al. 2024

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“…S5 0716+714, 3C 273, and 3C 279 were observed in the J, H, and K infrared bands with using the 200-inch Palomar Hale telescope and the WIRC+Pol 5 instrument (Tinyanont et al 2019a,b;Millar-Blanchaer et al 2021;Masiero et al 2022); the Kanata telescope using the Hiroshima Optical and Near-InfraRed camera (HONIR, Kawabata et al 1999;Akitaya et al 2014); and the IR camera MIMIR 6 (Clemens et al 2012) at the Perkins Telescope (PTO, Flagstaff, AZ). In the optical, all the sources we observed in B, V, R, I bands by the AZT-8 & LX-200 telescopes (St. Petersburg University); Calar Alto and Sierra Nevada observatories; DIPOL-2 polarimeter at the Haleakala observatory T60 telescope (Piirola 1973;Kosenkov et al 2017;Berdyugin et al 2018Berdyugin et al , 2019Piirola et al 2021); HONIR at the Kanata telescope; Alhambra Faint Object Spectrograph and Camera (ALFOSC) at the Nordic Optical Telescope (Hovatta et al 2016; 2018), and the RoboPol polarimeters at the Skinakas observatory (Panopoulou et al 2015;Ramaprakash et al 2019;Blinov et al 2021a)…”

Section: Appendixmentioning

confidence: 99%

Observations of 4U 1626–67 with the Imaging X-Ray Polarimetry Explorer

Marshall¹,

Ng²,

Rogantini³

et al. 2022

ApJ

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We present measurements of the polarization of X-rays in the 2–8 keV band from the pulsar in the ultracompact low-mass X-ray binary 4U 1626–67 using data from the Imaging X-Ray Polarimetry Explorer (IXPE). The 7.66 s pulsations were clearly detected throughout the IXPE observations as well as in the NICER soft X-ray observations, which we used as the basis for our timing analysis and to constrain the spectral shape over the 0.4–10 keV energy band. Chandra HETGS high-resolution X-ray spectra were also obtained near the times of the IXPE observations for firm spectral modeling. We found an upper limit on the pulse-averaged linear polarization of <4% (at 95% confidence). Similarly, there was no significant detection of polarized flux in pulse phase intervals when subdividing the bandpass by energy. However, spectropolarimetric modeling over the full bandpass in pulse phase intervals provided a marginal detection of polarization of the power-law spectral component at the 4.8% ± 2.3% level (90% confidence). We discuss the implications concerning the accretion geometry onto the pulsar, favoring two-component models of the pulsed emission.

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“…It collects light in a specific direction, making it a polarimeter, filter, or splitter. Due to small cubage, corrosion resistance, and easy demodulation, coupling zone distortion can affect output light ratio, low cost, and anti-EMI [28], [29]. Semiconductor quantum dots (QDs) have become an alternative material in light-emitting diodes, wavelength conversions, or even optical amplifiers [30].…”

Section: Introductionmentioning

confidence: 99%

Investigation of coupling loss caused by misalignment in optical fiber

et al. 2023

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In a fiber optic communication system, optical fiber is used as a transmission medium consisting of a flexible filament that guides the optical signal to be transmitted from the transmitter to the receiver or vice versa. Like any other communication medium, the optical fiber cable faces some losses that can be caused by the material and length of the fiber. One of the main reasons for losses in optical communication systems is misalignment during the fiber to fiber joining process. This type of loss is also known as coupling loss, which is caused by an imperfect physical connection between two fibers. The coupling losses are most often caused by three misalignment issues: end gap displacement, lateral displacement, and angular displacement. The main goal of this article is to investigate coupling loss caused by misalignment in optical fiber using the Modicom 6 module. Before we can find a way to reduce the coupling losses in the fiber optic system, we need to have a concrete idea about the nature of coupling losses due to misalignment. An ideal fiber coupler should not lose light and should be insensitive to light dispersion.

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Optical Polarimetry: Methods, Instruments and Calibration Techniques

Cited by 11 publications

References 43 publications

Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory

Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory

Observations of 4U 1626–67 with the Imaging X-Ray Polarimetry Explorer

Investigation of coupling loss caused by misalignment in optical fiber

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