Nonparametric Model Calibration for Derivatives

Abergel, Frédéric; Combes, Rémy Tachet des; Zaatour, Riadh

doi:10.4236/jmf.2017.73030

Cited by 6 publications

(11 citation statements)

References 12 publications

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“…As mentioned in the several Planck papers [16][17][18] the DL07 and GNILC-derived SEDs are compatible with MBB spectrum, which is obtained empirically from Planck observations of dust. For optically thin sources (like M31) the MBB function is as follows…”

Section: The Modified Blackbody Spectrumsupporting

confidence: 74%

“…There is anti-correlation between T d and β reported by Planck collaboration. 16,17 The spectral index of dust increases with radius, which means, that dust emission properties depend on the temperature, and the heating rate of dust depends on the spectral index. The corresponding values of the optical depth in this case are given in Table 3 and Table 4.…”

Section: Dust Emission Optical Depthmentioning

confidence: 99%

“…For our analysis we use the silicate-graphite-PAH model proposed in 15 (hereafter DL07), as well as Planck's dust emission maps. According to Planck team, [16][17][18] these models are described by single modified blackbody spectrum (MBB), from which we obtain radial variation of dust emission optical depth, using Planck's dust emission map at three frequencies.…”

Section: Introductionmentioning

confidence: 99%

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The structure of galactic halos and the microwave temperature maps

Amekhyan

2019

Int. J. Mod. Phys. D

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The study of Planck microwave temperature maps towards several nearby spiral edge-on galaxies had revealed frequency independent temperature asymmetry of Doppler origin in their halos. On an example of M31, as of relatively detailed studied galaxy, the contribution of the dust component in that effect is studied using the models of dust emission and the phenomenological profiles of the dark matter configurations. The results are in accordance with those obtained from the microwave temperature asymmetry data, thus indicating the possible contribution of dust among other radiation mechanisms in revealing the dark halo parameters.

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Section: The Modified Blackbody Spectrumsupporting

confidence: 74%

Section: Dust Emission Optical Depthmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The structure of galactic halos and the microwave temperature maps

Amekhyan

2019

Int. J. Mod. Phys. D

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“…The algorithm utilizes the GW localization map, an estimate of the event distance, and a model of the expected optical emission (e.g., Barnes & Kasen 2013). This information is folded in with observational information, including a map of sky brightness (using the DES sky brightness model; Neilsen 2012), the atmospheric transmission (using information on airmass and the interstellar dust extinction from Planck; Abergel et al 2014), the expected seeing (from scaling laws with airmass and wavelength), and the confusion-limit probability (based on stellar density maps) to produce a full source-detection probability as a function of sky location. We used this map to observe the highest probability region that included area both inside and outside the DES footprint.…”

Section: Observing Strategymentioning

confidence: 99%

A Dark Energy Camera Search for an Optical Counterpart to the First Advanced Ligo Gravitational Wave Event Gw150914

Soares-Santos¹,

Kessler²,

Berger³

et al. 2016

ApJL

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We report initial results of a deep search for an optical counterpart to the gravitational wave event GW150914, the first trigger from the Advanced LIGO gravitational wave detectors. We used the Dark Energy Camera (DECam) to image a 102 deg 2 area, corresponding to 38% of the initial trigger highprobability sky region and to 11% of the revised high-probability region. We observed in i and z bands at 4-5, 7, and 24 days after the trigger. The median 5σ point-source limiting magnitudes of our search images are i = 22.5 and z = 21.8 mag. We processed the images through a difference-imaging pipeline using templates from pre-existing Dark Energy Survey data and publicly available DECam data. Due to missing template observations and other losses, our effective search area subtends 40 deg 2 , corresponding to 12% total probability in the initial map and 3% of the final map. In this area, we search for objects that decline significantly between days 4-5 and day 7, and are undetectable by day 24, finding none to typical magnitude limits of i = 21.5, 21.1, 20.1 for object colors (i − z) = 1, 0, −1, respectively. Our search demonstrates the feasibility of a dedicated search program with DECam and bodes well for future research in this emerging field.

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“…It is notable generalization of Yang-Mills theories instead of using an addition auxiliary field to the gauge field, one can use the non-local action and cause to useful results in gauge field theories scenario [56]. We should emphasise for such mechanism in comparison to the canonical and local scalar field approach, by considering observations includes of Planck 2013 [59], W M AP 9 + eCM B + BAO + H 0 data sets in addition to BICEP 2 data surveying [57,58], our results are in good agreement. The paper has been planned in the following form: In Sec.1 which includes of above discussions we have introduction.…”

Section: Introductionmentioning

confidence: 99%

Non-local scalar fields inflationary mechanism in light of Planck 2013

Sheikhahmadi

Ghorbani

Saaidi

2015

Astrophys Space Sci

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A generalization of the canonical and non-canonical theory of inflation is introduced in which the kinetic energy term in action is written as non-local term. The inflationary universe within the framework of considering this non-locality will be studied. To investigate the effects of non-locality on the inflationary parameters we consider two well known models of inflationary scenario includes of chaotic and exponential inflation proposals. For such scenarios some important parameters include slow roll parameters, scalar and tensor power spectra, spectral indices, the tensor-to-scalar ratio and so on for both mentioned models, chaotic and exponential inflationary scenarios, will be calculated. Also the Hamilton-Jacobi formalism, as an easiest way to study the effect of perturbation based on e-folding number N , to investigate inflationary attractors will be used. The free theoretical parameters of this model will be compared with observations by means of Planck 2013, W M AP 9 + eCM B + BAO + H 0 data sets in addition to BICEP 2 data surveying. It will be shown that our theoretical results are in acceptable range in comparison to observations. For instance the tensor-to-scalar ratio for exponential potential, by considering BICEP 2 is in best agreement in comparison with chaotic inflation.

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Nonparametric Model Calibration for Derivatives

Cited by 6 publications

References 12 publications

The structure of galactic halos and the microwave temperature maps

The structure of galactic halos and the microwave temperature maps

A Dark Energy Camera Search for an Optical Counterpart to the First Advanced Ligo Gravitational Wave Event Gw150914

Non-local scalar fields inflationary mechanism in light of Planck 2013

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