Kapitel 7: Quantenwelt und Quantencomputer (Feynman et al.)

Mainzer, Klaus

doi:10.17104/9783406661310-118

Cited by 31 publications

(37 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This data is summarised in Table 3. We have extracted the NIR photometry and observing dates from 2MASS (Skrutskie et al 2006), UGPS (Lucas et al 2008) data release DR11, as well as the MIR observations from NEOWISE (Mainzer et al 2011(Mainzer et al , 2014 in the W1-and W2-bands from the WISE satellite (Wright et al 2010). For the latter we have averaged all the measurements taken over the usually one to three day repeated visits for the source and used the RMS as the uncertainty.…”

Section: Literature Nir and Mir Data For V1490 Cygmentioning

confidence: 99%

A survey for variable young stars with small telescopes: II – mapping a protoplanetary disc with stable structures at 0.15 au

Evitts

Froebrich

Scholz

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The HOYS citizen science project conducts long-term, multifilter, high-cadence monitoring of large YSO samples with a wide variety of professional and amateur telescopes. We present the analysis of the light curve of V1490 Cyg in the Pelican Nebula. We show that colour terms in the diverse photometric data can be calibrated out to achieve a median photometric accuracy of 0.02 mag in broad-band filters, allowing detailed investigations into a variety of variability amplitudes over time-scales from hours to several years. Using Gaia DR2, we estimate the distance to the Pelican Nebula to be 870 $^{+70}_{-55}$ pc. V1490 Cyg is a quasi-periodic dipper with a period of 31.447 ± 0.011 d. The obscuring dust has homogeneous properties, and grains larger than those typical in the ISM. Larger variability on short time-scales is observed in U and Rc−H α, with U amplitudes reaching 3 mag on time-scales of hours, indicating that the source is accreting. The H α equivalent width and NIR/MIR colours place V1490 Cyg between CTTS/WTTS and transition disc objects. The material responsible for the dipping is located in a warped inner disc, about 0.15 au from the star. This mass reservoir can be filled and emptied on time-scales shorter than the period at a rate of up to 10−10 M⊙ yr−1, consistent with low levels of accretion in other T Tauri stars. Most likely, the warp at this separation from the star is induced by a protoplanet in the inner accretion disc. However, we cannot fully rule out the possibility of an AA Tau-like warp, or occultations by the Hill sphere around a forming planet.

show abstract

Section: Literature Nir and Mir Data For V1490 Cygmentioning

confidence: 99%

A survey for variable young stars with small telescopes: II – mapping a protoplanetary disc with stable structures at 0.15 au

Evitts

Froebrich

Scholz

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The WISE team has released two all sky catalogues: the 9 month cryogenic phase of the mission led to the WISE All-Sky ("AllSky") Data Release; while the WISE AllWISE Data Release ("AllWISE") combines the AllSky data with the NEOWISE program (Mainzer et al 2011). The resulting AllWISE dataset is deeper in the two shorter WISE-bands (5σ point-source sensitivities now 0.054 and 0.071 mJy), and the data processing algorithms were improved in all four Wbands.…”

Section: Parent Datasetmentioning

confidence: 99%

Extremely red quasars from SDSS, BOSS andWISE: classification of optical spectra

Ross

Hamann

Zakamska

et al. 2015

Mon. Not. R. Astron. Soc.

104

View full text Add to dashboard Cite

Quasars with extremely red infrared-to-optical colours are an interesting population that can test ideas about quasar evolution as well as orientation, obscuration and geometric effects in the so-called AGN unified model. To identify such a population we match the quasar catalogues of the Sloan Digital Sky Survey (SDSS), the Baryon Oscillation Spectroscopic Survey (BOSS) to the Wide-Field Infrared Survey Explorer (WISE) to identify quasars with extremely high infrared-to-optical ratios. We identify 65 objects with r AB − W 4 Vega > 14 mag (i.e., F ν (22µm)/F ν (r) > ∼ 1000). This sample spans a redshift range of 0.28 < z < 4.36 and has a bimodal distribution, with peaks at z ∼ 0.8 and z ∼ 2.5. It includes three z > 2.6 objects that are detected in the W 4-band but not W 1 or W 2 (i.e., "W1W2-dropouts"). The SDSS/BOSS spectra show that the majority of the objects are reddened Type 1 quasars, Type 2 quasars (both at low and high redshift) or objects with deep low-ionization broad absorption lines (BALs) that suppress the observed r-band flux. In addition, we identify a class of Type 1 permitted broad-emission line objects at z ≃ 2 − 3 which are characterized by emission line rest-frame equivalent widths (REWs) of 150Å, much larger than those of typical quasars. In particular, 55% (45%) of the non-BAL Type 1s with measurable CIV in our sample have REW(CIV) > 100 (150)Å, compared to only 5.8% (1.3%) for non-BAL quasars in BOSS. These objects often also have unusual line ratios, such as very high N v/Lyα ratios. These large REWs might be caused by suppressed continuum emission analogous to Type 2 quasars; however, there is no obvious mechanism in standard Unified Models to suppress the continuum without also obscuring the broad emission lines.

show abstract

“…In this study, we used the AllWISE data release, which combines the 4-band cryogenic phase with the NEOWISE post-cryo phase (Mainzer et al 2011). This data release is deeper than the previous all-sky data release by roughly a factor of two in W1 and W2 bands as the NEOWISE post-cryo phase only used these two bands.…”

Section: Wise Datamentioning

confidence: 99%

Measurement of the Integrated Sachs–wolfe Effect Using the Allwise Data Release

Shajib

Wright²

2016

ApJ

View full text Add to dashboard Cite

One of the physical features of a dark-energy-dominated universe is the integrated Sachs-Wolfe (ISW) effect on the cosmic microwave background (CMB) radiation, which gives us a direct observational window to detect and study dark energy. The AllWISE data release of the Wide-field Infrared Survey Explorer (WISE) has a large number of point sources, which span over a wide redshift range including where the ISW effect is maximized. AllWISE data is thus very well-suited for the ISW effect studies. In this study, we cross-correlate AllWISE galaxy and active galactic nucleus (AGN) overdensities with the Wilkinson Microwave Anisotropy Probe CMB temperature maps to detect the ISW effect signal. We calibrate the biases for galaxies and AGNs by crosscorrelating the galaxy and AGN overdensities with the Planck lensing convergence map. We measure the ISW effect signal amplitudes relative to the ΛCDM expectation of A = 1 to be A = 1.18 ± 0.36 for galaxies and A = 0.64 ± 0.74 for AGNs . The detection significances for the ISW effect signal are 3.3σ and 0.9σ for galaxies and AGNs respectively giving a combined significance of 3.4σ. Our result is in agreement with the ΛCDM model.

show abstract

Kapitel 7: Quantenwelt und Quantencomputer (Feynman et al.)

Cited by 31 publications

References 0 publications

A survey for variable young stars with small telescopes: II – mapping a protoplanetary disc with stable structures at 0.15 au

A survey for variable young stars with small telescopes: II – mapping a protoplanetary disc with stable structures at 0.15 au

Extremely red quasars from SDSS, BOSS andWISE: classification of optical spectra

Measurement of the Integrated Sachs–wolfe Effect Using the Allwise Data Release

Contact Info

Product

Resources

About