Abstract:A nautilid faunule of seven specimens, comprising Eutrephoceras bouchardianum (d’Orbigny, 1840), Cymatoceras deslongchampsianum (d’Orbigny, 1840), and Cymatoceras tourtiae (Schlüter, 1876) is described from a condensed middle Cenomanian interval at Annopol, Poland. C. tourtiae is recorded for the first time in Poland. The studied material consists of reworked phosphatised internal moulds of phragmocones, which may be of early or middle Cenomanian age, given the stratigraphic range of the associated ammonites. … Show more
“…As recently pointed out by Condon et al (2012), the integrated light There is a clear divergence occurring at ≈175 mJy, where the integrated light from the NVSS data appears to be increase more rapidly towards lower flux densities compared to the curve from Condon et al (2012). This location of the divergence is exactly where the data used in the (Condon et al 2012) study switched from NRAO 91 m data (Machalski 1978) to various WSRT and VLA interferometric observations (see Condon 1984a) requiring large correction factors for incompleteness caused by primary beam attenuation, as well as for partial source resolution by the smaller synthesized beams.…”
Section: Comparison With the Arcade 2 Excesssupporting
confidence: 51%
“…The cumulative histograms appear to diverge at ≈175 mJy, where the 1.4 GHz brightness temperature using the NVSS data begins to increase more rapidly towards lower flux densities relative to the histogram from Condon et al (2012). The location of the divergence is exactly where the data used in the Condon et al (2012) study switched from single-dish, NRAO 91 m data (Machalski 1978) to various WSRT and VLA interferometric observations compiled by Condon (1984a).…”
Section: Comparison With Other Work At 14 Ghzmentioning
We conduct a stacking analysis using the combination of 1.4 GHz detections in the NRAO VLA Sky Survey (NVSS) and Planck all-sky maps to estimate the differential source counts down to the few 100 μJy level at 30, 44, 70, and 100 GHz. Using these source count estimates, we are able to measure the integrated extragalactic background light from discrete sources at these frequencies for comparison with the fit to the total radio sky measurements from ARCADE 2. By integrating down to a 1.4 GHz flux density of ≈2 μJy, we measure integrated, extragalactic brightness temperatures from discrete sources of 105.63±10.56 mK, 21.76±3.09 μK, 8.80±0.95 μK, 2.59±0.27 μK, and 1.15±0.10 μk at 1.4, 30, 44, 70, and 100 GHz, respectively. Our measurement at 1.4 GHz is slightly larger than previous measurements, most likely due to using NVSS data compared with older interferometric data in the literature, but it still remains a factor of ≈4.5 below that required to account for the excess extragalactic sky brightness measured at 1.4 GHz by ARCADE 2. The fit to ARCADE 2 total extragalactic sky brightness measurements is also a factor of ≈8.6, 6.6, 6.2, and 4.9 times brighter than what we estimate from discrete sources at 30, 44, 70, and 100 GHz, respectively. The extragalactic sky spectrum (i.e., T b ∝ ν β ) from discrete sources appears to flatten with increasing frequency, having a spectral index of β=−2.82±0.06 between 1.4 and 30 GHz, flattening to β=−2.39±0.12 between 30 and 100 GHz. We estimate that the spectral flattening most likely arises from a combination of gigahertz-peaked sources and the hardening of the spectra of radio-detected sources at higher frequencies, particularly at faint flux densities. However, the precise origin of a hard component of energetic electrons responsible for the emission remains unclear.
“…As recently pointed out by Condon et al (2012), the integrated light There is a clear divergence occurring at ≈175 mJy, where the integrated light from the NVSS data appears to be increase more rapidly towards lower flux densities compared to the curve from Condon et al (2012). This location of the divergence is exactly where the data used in the (Condon et al 2012) study switched from NRAO 91 m data (Machalski 1978) to various WSRT and VLA interferometric observations (see Condon 1984a) requiring large correction factors for incompleteness caused by primary beam attenuation, as well as for partial source resolution by the smaller synthesized beams.…”
Section: Comparison With the Arcade 2 Excesssupporting
confidence: 51%
“…The cumulative histograms appear to diverge at ≈175 mJy, where the 1.4 GHz brightness temperature using the NVSS data begins to increase more rapidly towards lower flux densities relative to the histogram from Condon et al (2012). The location of the divergence is exactly where the data used in the Condon et al (2012) study switched from single-dish, NRAO 91 m data (Machalski 1978) to various WSRT and VLA interferometric observations compiled by Condon (1984a).…”
Section: Comparison With Other Work At 14 Ghzmentioning
We conduct a stacking analysis using the combination of 1.4 GHz detections in the NRAO VLA Sky Survey (NVSS) and Planck all-sky maps to estimate the differential source counts down to the few 100 μJy level at 30, 44, 70, and 100 GHz. Using these source count estimates, we are able to measure the integrated extragalactic background light from discrete sources at these frequencies for comparison with the fit to the total radio sky measurements from ARCADE 2. By integrating down to a 1.4 GHz flux density of ≈2 μJy, we measure integrated, extragalactic brightness temperatures from discrete sources of 105.63±10.56 mK, 21.76±3.09 μK, 8.80±0.95 μK, 2.59±0.27 μK, and 1.15±0.10 μk at 1.4, 30, 44, 70, and 100 GHz, respectively. Our measurement at 1.4 GHz is slightly larger than previous measurements, most likely due to using NVSS data compared with older interferometric data in the literature, but it still remains a factor of ≈4.5 below that required to account for the excess extragalactic sky brightness measured at 1.4 GHz by ARCADE 2. The fit to ARCADE 2 total extragalactic sky brightness measurements is also a factor of ≈8.6, 6.6, 6.2, and 4.9 times brighter than what we estimate from discrete sources at 30, 44, 70, and 100 GHz, respectively. The extragalactic sky spectrum (i.e., T b ∝ ν β ) from discrete sources appears to flatten with increasing frequency, having a spectral index of β=−2.82±0.06 between 1.4 and 30 GHz, flattening to β=−2.39±0.12 between 30 and 100 GHz. We estimate that the spectral flattening most likely arises from a combination of gigahertz-peaked sources and the hardening of the spectra of radio-detected sources at higher frequencies, particularly at faint flux densities. However, the precise origin of a hard component of energetic electrons responsible for the emission remains unclear.
“…1A). The reader is referred to Walaszczyk (1987), Machalski and Wilmsen (2015), and Dubicka and Machalski (2017) for more detailed descriptions of this interval.…”
Section: General Backgroundmentioning
confidence: 99%
“…This material originates from the upper Albian-middle Cenomanian part of the Cretaceous sedimentary succession exposed at Annopol, central Poland. This contribution is an addition to a series of papers on the Cretaceous biota from Annopol, resulting from recent exploration of this important Polish "Fossil-Lagerstätte" (Machalski and Kennedy 2013;Machalski and Martill 2013;Popov and Machalski 2014;Kennedy and Machalski 2015;Kapuścińska and Machalski 2015;Fraaije et al 2015;Machalski and Wilmsen 2015;Bardet et al 2016;Machalski and Olszewska-Nejbert 2016;Dubicka and Machalski 2017;Siversson and Machalski 2017). An important part of the studied material comes from the collection of late Prof. Andrzej Radwański, who was so successfully involved in earlier investigations of the Annopol fossils, depositional environments, and biostratigraphy (Radwański 1968;Radwański 1983, 1989).…”
ABSTRACT:Madzia, D. and Machalski, M. 2017. Isolated pliosaurid teeth from the Albian-Cenomanian (Cretaceous) of Annopol, Poland. Acta Geologica Polonica, 67 (3), 393-403. Warszawa.Brachauchenine pliosaurids were a cosmopolitan clade of macropredatory plesiosaurs that are considered to represent the only pliosaurid lineage that survived the faunal turnover of marine amniotes during the JurassicCretaceous transition. However, the European record of the Early to early Late Cretaceous brachauchenines is largely limited to isolated tooth crowns, most of which have been attributed to the classic Cretaceous taxon Polyptychodon. Nevertheless, the original material of P. interruptus, the type species of Polyptychodon, was recently reappraised and found undiagnostic. Here, we describe a collection of twelve pliosaurid teeth from the upper Albian-middle Cenomanian interval of the condensed, phosphorite-bearing Cretaceous succession at Annopol, Poland. Eleven of the studied tooth crowns, from the Albian and Cenomanian strata, fall within the range of the morphological variability observed in the original material of P. interruptus from the Cretaceous of England. One tooth crown from the middle Cenomanian is characterized by a gently subtrihedral cross-section. Similar morphology has so far been described only for pliosaurid teeth from the Late Jurassic and Early Cretaceous. Even though it remains impossible to precisely settle the taxonomic distinctions, the studied material is considered to be taxonomically heterogeneous.
“…2d). The phosphatic horizon contains a biostratigraphically mixed ammonite assemblage, ranging from the middle Albian Hoplites dentatus Zone to the lowermost upper upper Albian Mortoniceras fallax Zone (Marcinowski & Radwański, 1983, 1989; Machalski & Kennedy, 2013; Kennedy & Machalski, 2015; see Table 1 for the ammonite zonations used in the present paper). Figure 2. Close-up views of the upper Albian interval of the Annopol successions to show the bioturbated nature of the phosphatic layer at the top of unit 3 (a, b) and discrete burrows filled with the Cenomanian marls in this unit (c) and near the top of the underlying unit 2 (d).…”
A condensed succession at Annopol is of key importance for the mid-Cretaceous palaeontology and palaeobiogeography in Poland. Here, the planktonic and benthic foraminifera from the Albian and Cenomanian intervals are studied. The local foraminiferal record is strongly influenced by burrowers. On the one hand, piping down of the foraminiferal tests through burrows disturbed the original succession, for example by introduction of the Cenomanian foraminifera into the Albian phosphorite horizon. On the other hand, the foraminifera in the burrow fills near the base of the Cenomanian provide the sole piece of evidence of a lower upper Cenomanian unit lost from the record by erosion. Changes in foraminiferal assemblages allow for the interpretation of the succession in terms of bathymetry and biological productivity. The highest rate of primary production is deduced for the Albian phosphorite horizon. Integration of foraminiferal and ammonite biostratigraphy with sedimentology allows for the comparison of a pattern of sea-level oscillations recorded at Annopol with the relevant portion of the classic graph of sea-level changes for the British Isles. It turns out that all important elements of the British curve, that is, transgressive peaks and regressive troughs or lows, left their distinctive, albeit highly residual, record in the Annopol succession. This study demonstrates that even extremely condensed marine deposits, such as those at Annopol, may provide a foraminiferal record of better quality, order and resolution than conventionally anticipated.
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