Millimeter and Radio Observations of z~6 Quasars

We present millimeter and radio observations of 13 SDSS quasars at reshifts z~6. We observed eleven of them with the Max-Planck Millimeter Bolometer Array (MAMBO-2) at the IRAM 30m-telescope at 250 GHz and all of them with the Very Large Array (VLA) at 1.4 GHz. Four sources are detected by MAMBO-2 and six are detected by the VLA at >=3 sigma level. These sources, together with another 6 published in previous papers,yield a submillimeter/millimeter and radio observed SDSS quasar sample at z~6. We use this sample to investigate the far-infrared (FIR) andradio properties of optically bright quasars in the early universe. We compare this sample to lower redshift samples of quasars observed inthe submillimeter and millimeter wavelengths ((sub)mm), and find that the distribution of the FIR to B band optical luminosity ratio (L_FIR/L_B) is similar from z~2 to 6. We find a weak correlation between the FIR luminosity (L_FIR) and B band optical luminosity (L_B) byincluding the (sub)mm observed samples at all redshifts. Some strong (sub)mm detections in the z~6 sample have radio-to-FIR ratios within the range defined by star forming galaxies, which suggests possible co-eval star forming activity with the powerful AGN in these sources. We calculate the rest frame radio to optical ratios (R*_1.4=L_{v, 1.4GHz}/L_{v, 4400A}) for all of the VLA observed sources in the z~6 quasar sample. Only one radio detection in this sample, J083643.85+005453.3, has R*_1.4~40 and can be considered radio loud. There are no strong radio sources (R*_1.4>=100) among these SDSS quasars at z~6. These data are consistent with, although do not set strong constraints on, a decreasing radio-loud quasar fraction with increasing redshift.Comment: 27 pages including 6 figures. AJ accepte

Millimeter and Radio Observations of z~6 Quasars

We present millimeter and radio observations of 13 SDSS quasars at reshifts z~6. We observed eleven of them with the Max-Planck Millimeter Bolometer Array (MAMBO-2) at the IRAM 30m-telescope at 250 GHz and all of them with the Very Large Array (VLA) at 1.4 GHz. Four sources are detected by MAMBO-2 and six are detected by the VLA at >=3 sigma level. These sources, together with another 6 published in previous papers,yield a submillimeter/millimeter and radio observed SDSS quasar sample at z~6. We use this sample to investigate the far-infrared (FIR) andradio properties of optically bright quasars in the early universe. We compare this sample to lower redshift samples of quasars observed inthe submillimeter and millimeter wavelengths ((sub)mm), and find that the distribution of the FIR to B band optical luminosity ratio (L_FIR/L_B) is similar from z~2 to 6. We find a weak correlation between the FIR luminosity (L_FIR) and B band optical luminosity (L_B) byincluding the (sub)mm observed samples at all redshifts. Some strong (sub)mm detections in the z~6 sample have radio-to-FIR ratios within the range defined by star forming galaxies, which suggests possible co-eval star forming activity with the powerful AGN in these sources. We calculate the rest frame radio to optical ratios (R*_1.4=L_{v, 1.4GHz}/L_{v, 4400A}) for all of the VLA observed sources in the z~6 quasar sample. Only one radio detection in this sample, J083643.85+005453.3, has R*_1.4~40 and can be considered radio loud. There are no strong radio sources (R*_1.4>=100) among these SDSS quasars at z~6. These data are consistent with, although do not set strong constraints on, a decreasing radio-loud quasar fraction with increasing redshift.Comment: 27 pages including 6 figures. AJ accepte

Coordinated capacity and demand management in a redesigned air traffic management value-chain

We present a re-designed European Air Traffic Management value-chain, with a new role for the Network Manager, which coordinates capacity and demand management decisions, using economic instruments for both areas. A conceptual and mathematical model supports decision-making in that process, focusing on capacity management decisions taken at the strategic level. Total costs are minimized by jointly managing sector-opening schemes and trajectory assignments. A large-scale case study demonstrates clear trade-offs between the volume of capacity ordered and the scope of necessary demand management actions. In addition, the comparison against a baseline, which resembles the current system, shows that with the proposed concept less capacity is needed to serve the same demand, resulting in lower total cost for Aircraft Operators

Gas dynamics of a luminous zz = 6.13 quasar ULAS J1319++0950 revealed by ALMA high resolution observations

We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 $\mu$m fine structure line emission towards a far-infrared-luminous quasar, ULAS J131911.29$+$095051.4 at $z=6.13$, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution $\sim$ $0.3$, and resolve both the dust continuum and the [C II] line emission on few kpc scales. The [C II] line emission is more irregular than the dust continuum emission which suggests different distributions between the dust and [C II]-emitting gas. The combined data confirm the [C II] velocity gradient that we previously detected in lower resolution ALMA image from Cycle 0 data alone. We apply a tilted ring model to the [C II] velocity map to obtain a rotation curve, and constrain the circular velocity to be 427 $\pm$ 55 km s$^{-1}$ at a radius of 3.2 kpc with an inclination angle of 34$^\circ$. We measure the dynamical mass within the 3.2 kpc region to be 13.4$_{-5.3}^{+7.8}$ $\times 10^{10}\,M_{\odot}$. This yields a black hole and host galaxy mass ratio of 0.020$_{-0.007}^{+0.013}$, which is about 4$_{-2}^{+3}$ times higher than the present-day $M_{\rm BH}$/$M_{\rm bulge}$ ratio. This suggests that the supermassive black hole grows the bulk of its mass before the formation of the most of stellar mass in this quasar host galaxy in the early universe.Comment: 24 pages, 5 figures, accepted for publication in Ap

Carbon and nitrogen pools in thermokarst-affected permafrost landscapes in Arctic Siberia

Ice rich Yedoma-dominated landscapes store considerable amounts of organic carbon (C) and nitrogen (N) and are vulnerable to degradation under climate warming. We investigate the C and N pools in two thermokarst-affected Yedoma landscapes – on Sobo-Sise Island and on Bykovsky Peninsula in the North of East Siberia. Soil cores up to three meters depth were collected along geomorphic gradients and analysed for organic C and N contents. A high vertical sampling density in the profiles allowed the calculation of C and N stocks for short soil column intervals and enhanced understanding of within-core parameter variability. Profile-level C and N stocks were scaled to the landscape level based on landform classifications from five-meter resolution, multispectral RapidEye satellite imagery. Mean landscape C and N storage in the first meter of soil for Sobo-Sise Island is estimated to be 20.2 kg C m−2 and 1.8 kg N m−2 and for Bykovsky Peninsula 25.9 kg C m−2 and 2.2 kg N m−2. Radiocarbon dating demonstrates the Holocene age of thermokarst basin deposits but also suggests the presence of thick Holocene aged cover layers which can reach up to two meters on top of intact Yedoma landforms. Reconstructed sedimentation rates of 0.10 mm yr−1–0.57 mm yr−1 suggest sustained mineral soil accumulation across all investigated landforms. Both Yedoma and thermokarst landforms are characterized by limited accumulation of organic soil layers (peat). We further estimate that an active layer deepening by about 100 cm will increase organic C availability in a seasonally thawed state in the two study areas by ~ 5.8 Tg (13.2 kg C m−2). Our study demonstrates the importance of increasing the number of C and N storage inventories in ice-rich Yedoma and thermokarst environments in order to account for high variability of permafrost and thermokarst environments in pan-permafrost soil C and N pool estimates

Probing the interstellar medium and star formation of the Most Luminous Quasar at z=6.3

We report new IRAM/PdBI, JCMT/SCUBA-2, and VLA observations of the ultraluminous quasar SDSSJ010013.02+280225.8 (hereafter, J0100+2802) at z=6.3, which hosts the most massive supermassive black hole (SMBH) of 1.24x10^10 Msun known at z>6. We detect the [C II] 158 $\mu$m fine structure line and molecular CO(6-5) line and continuum emission at 353 GHz, 260 GHz, and 3 GHz from this quasar. The CO(2-1) line and the underlying continuum at 32 GHz are also marginally detected. The [C II] and CO detections suggest active star formation and highly excited molecular gas in the quasar host galaxy. The redshift determined with the [C II] and CO lines shows a velocity offset of ~1000 km/s from that measured with the quasar Mg II line. The CO (2-1) line luminosity provides direct constraint on the molecular gas mass which is about (1.0+/-0.3)x10^10 Msun. We estimate the FIR luminosity to be (3.5+/-0.7)x10^12 Lsun, and the UV-to-FIR spectral energy distribution of J0100+2802 is consistent with the templates of the local optically luminous quasars. The derived [C II]-to-FIR luminosity ratio of J0100+2802 is 0.0010+/-0.0002, which is slightly higher than the values of the most FIR luminous quasars at z~6. We investigate the constraint on the host galaxy dynamical mass of J0100+2802 based on the [C II] line spectrum. It is likely that this ultraluminous quasar lies above the local SMBH-galaxy mass relationship, unless we are viewing the system at a small inclination angle.Comment: 19 pages, 4 figures, published by the Astrophysical Journal, minimal changes in acknowledgement to match the published versio

Adjusting for Network Size and Composition Effects in Exponential-Family Random Graph Models

Exponential-family random graph models (ERGMs) provide a principled way to model and simulate features common in human social networks, such as propensities for homophily and friend-of-a-friend triad closure. We show that, without adjustment, ERGMs preserve density as network size increases. Density invariance is often not appropriate for social networks. We suggest a simple modification based on an offset which instead preserves the mean degree and accommodates changes in network composition asymptotically. We demonstrate that this approach allows ERGMs to be applied to the important situation of egocentrically sampled data. We analyze data from the National Health and Social Life Survey (NHSLS).Comment: 37 pages, 2 figures, 5 tables; notation revised and clarified, some sections (particularly 4.3 and 5) made more rigorous, some derivations moved into the appendix, typos fixed, some wording change