GEOMAGIA50.v3: 2. A new paleomagnetic database for lake and marine sediments
© Brown et al.; licensee Springer. 2015
Received: 4 February 2015
Accepted: 17 April 2015
Published: 12 May 2015
GEOMAGIA50.v3 for sediments is a comprehensive online database providing access to published paleomagnetic, rock magnetic, and chronological data obtained from lake and marine sediments deposited over the past 50 ka. Its objective is to catalogue data that will improve our understanding of changes in the geomagnetic field, physical environments, and climate.
GEOMAGIA50.v3 for sediments builds upon the structure of the pre-existing GEOMAGIA50 database for magnetic data from archeological and volcanic materials. A strong emphasis has been placed on the storage of geochronological data, and it is the first magnetic archive that includes comprehensive radiocarbon age data from sediments. The database will be updated as new sediment data become available.
The web-based interface for the sediment database is located at http://geomagia.gfz-potsdam.de/geomagiav3/SDquery.php. This paper is a companion to Brown et al. (Earth Planets Space doi:10.1186/s40623-015-0232-0, 2015) and describes the data types, structure, and functionality of the sediment database.
KeywordsGeomagnetism Paleomagnetism Sediment magnetism Rock magnetism Environmental magnetism Database GEOMAGIA50
The aim of the GEOMAGIA50 database is to allow easy access to paleomagnetic data from the past 50 ka. Previous versions of the database (Donadini et al. 2006; Korhonen et al. 2008) stored palaeomagnetic data from archeological materials and lavas alone; however, paleomagnetic, rock magnetic, and chronological data from sediments deposited over the past 50 ka have broad applications across the geosciences. These include understanding past changes in the geomagnetic field, physical environments, climate, and anthropogenic impact.
In a companion paper (Brown et al. 2015), the latest modifications to the general structure of the GEOMAGIA50 database and more specific changes to the archeo/volcanic database are described. This paper addresses the scientific rationale, design, and function of the newly implemented sediment database.
Paleomagnetic data from sediments complement the wealth of data from archeological and volcanic materials covering the same period already stored within the GEOMAGIA50 database (Brown et al. 2015). Furthermore, the amount of paleomagnetic data from archeological materials and lavas decreases greatly prior to 2 ka (see Brown et al. 2015; Donadini et al. 2009). Paleomagnetic data from sediments are therefore essential to our understanding of the temporal and spatial evolution of the geomagnetic field over longer time scales. In addition, the inclusion of rock magnetic and chronological data from sediments in GEOMAGIA50 expands the range of scientific problems that can be addressed by the database.
The quasi-continuous nature of sediments makes them an attractive source of information about temporal changes in the geomagnetic field. They augment archeomagnetic and volcanic data, which provide only spot readings of the paleomagnetic field and are often sparsely distributed in time (e.g., Guyodo and Valet 1999a). The joint analysis of sediment and archeomagnetic and/or lava data allows the resolution of a greater degree of complexity in field behavior (e.g., Korte and Constable 2005). This is true for not only the past 50 ka, but in the case of lavas, over other geomagnetically interesting times, such as during reversals (e.g., Brown et al. 2013; Coe and Glen 2004).
In recent years, paleomagnetic data from sediments have been incorporated into empirical models of the Holocene geomagnetic field (e.g., Korte and Constable 2005; Korte et al. 2009, 2011; Licht et al. 2013; Nilsson et al. 2014; Panovska 2012). Encouragingly, Holocene geomagnetic field models generate globally consistent time-averaged structures; however, in some studies, low-quality paleomagnetic data from sediments and/or erroneous age models can result in temporal ambiguities between records and therefore a distorted picture of the time-varying geomagnetic field. Providing more comprehensive data will enable a rigorous assessment of the factors that may influence these records and allow more realistic uncertainties to be assigned.
The power spectrum of geomagnetic dipole moment variations allows us to investigate the time necessary to average the geomagnetic field to obtain a stable time-average (if this exists). In addition, the distribution of power over the full range of frequencies applicable to the geomagnetic field has important statistical properties that can be compared with the output of numerical dynamo simulations (e.g., Davies and Constable 2014; Driscoll and Olson 2009; Olson et al. 2012; Sakuraba and Hamano 2007). This spans from measurements of short-term variations of the present day field, through satellite missions such as Swarm (Olsen et al. 2013) and observatory data (Reay et al. 2011), to paleomagnetic observations of superchrons, such as the Cretaceous Normal Superchron (e.g., Granot et al. 2012; Tarduno et al. 2001; Tauxe and Staudigel 2004). Ziegler and Constable (2011) investigated the power spectrum over the last 2 Ma (see Figure 1 for a composite spectrum derived from various sources including their estimate). However, they did not resolve discrepancies noted by Constable and Johnson (2005) among power spectra determined from various marine sediments at frequencies between 30 My −1 (30 ky) and 200 My −1 (5 ky). At the high-frequency end, Holocene field models provide some information (depending on the model resolution), but an important application of sediment data within GEOMAGIA50 will be to improve the paleomagnetic power spectrum over the intermediate frequency range.
At least two geomagnetic field excursions (Mono Lake/Auckland and Laschamp) have been recorded at a number of globally distributed locations between 10 and 50 ka (e.g., Laj and Channell 2007; Laj et al. 2014; Nowaczyk et al. 2012, 2013; Singer 2014). Studies on high sedimentation rate cores across the Laschamp excursion (e.g., Nowaczyk et al. 2012) have revealed an ever more detailed picture of surface field changes. Furthermore, additional excursion-like behavior has been noted at distinctly different times, e.g., the Hilina Pali/Tianchi excursion (Coe et al. 1978; Singer 2014; Singer et al. 2014; Teanby et al. 2002), occurring at approximately 17 ka (Singer et al. 2014). A better documentation of excursions is integral to a fuller understanding of geodynamo processes (Amit et al. 2010; Olson et al. 2011; Wicht 2005); the interaction between the geomagnetic field, the paleomagnetosphere, and space climate during times of extreme geomagnetic change (Constable and Korte 2006; Stadelmann et al. 2010; Vogt et al. 2007; and the dramatic modulation of cosmogenic isotopes such as 10Be and 14C, with associated implications for dating (e.g., Muscheler et al. 2014). However, the physical origin of excursions is unclear, with multiple mechanisms proposed (see Amit et al. 2010). Although modeling of the Laschamp excursion has been attempted (Leonhardt et al. 2009), the time span was restrictive and the number of sediment records used for the modeling limited. The first step to understanding the evolution of the geomagnetic field over this time is the compilation and assessment of all available sediment records.
Over the last 15 years, relative paleointensity data have been used to construct global and regional paleointensity stacks to aid in stratigraphic studies (e.g., Simon et al. 2012) and to broadly characterize the global geomagnetic field, including the field over the past 50 ka (e.g., SINT-800 (Guyodo and Valet 1999b); SINT-2000 (Valet et al. 2005); NAPIS (Laj et al. 2000); SAPIS (Stoner et al. 2002); GLOPIS (Laj et al. 2004); PISO-1500 (Channell et al. 2009); NOPAPIS-250 (Yamamoto et al. 2007); and PADM2M (Ziegler et al. 2011)). Roberts et al. 2013 noted non-trivial differences between some stacks for the past 40 ka and stated these differences were outside measurement errors or errors of the stacking procedures. The provision of a substantial amount of relative paleointensity and chronological data will allow refinement of such stacks over the past 50 ka, and corresponding rock magnetic data may aid in understanding if remanence acquisition processes vary among sediments from different environments.
In addition to improving our understanding of the geomagnetic field, the magnetic properties of lacustrine and marine sediments can aid our interpretation of environmental and climate change (see reviews by Liu et al. 2012 and Verosub and Roberts 1995). Variations in the mineralogy, concentration, and grain size of magnetic particle assemblages, either as input or through in situ processes, may be linked to changes in the local environment or climate. Climate may affect weathering, erosion, and sedimentation processes, resulting in distinct magnetominerological facies. In situ processes may be deduced from the identification of oxidation, dissolution, and growth of new magnetic minerals, such as sulphides (e.g., Frank et al. 2007; Nowaczyk 2011; Roberts et al. 2011; Snowball and Thompson 1988).
It has long been noted that fluctuations in concentration and magnetic grain size may be modulated by climate (e.g., Bloemendal and deMenocal 1989; Kent 1982; Peck et al. 1994). For example, variations in magnetic susceptibility have been observed to correlate with variations in δ 18O (e.g., Frank et al. 2013; Thouveny et al. 1994). Other magnetic parameters, such as the S-ratio (Bloemendal et al. 1992; Thompson and Oldfield 1986), have been demonstrated to be sensitive indicators of climate change (e.g., Meynadier et al. 1995; Snowball 1993). Furthermore, anthropogenic impact has been identified in rock magnetic records from lake and marine sediments around the world, reflecting deforestation, erosion rates, and changes in sediment delivery over the past approximately 4 ka and particulate pollution since approximately 1800 AD (see review by Snowball et al. 2014). The rock magnetic data within the database will allow a comprehensive assessment of the magnetic properties of sediments and their relationship to climate, environment, and anthropogenic impact.
Several databases provide paleomagnetic, rock magnetic, and chronological data; however, none that are currently maintained exclusively catalogue data from sediments over the past 50 ka. The SedDB database (www.earthchem.org/seddb) (Johansson et al. 2012), part of the IEDA Cooperative Agreement funded by the US National Science Foundation, contains a vast range of geochemical data from sediments; however, it contains no magnetic data. The GEOMAGIA50 database for sediments complements data available from the Magnetics Information Consortium (MagIC) database (https://earthref.org/MAGIC/) (Constable et al. 2006; Jarboe et al. 2012) and the International Association of Geomagnetism and Aeronomy (IAGA) absolute paleointensity database (PINT) (http://earth.liv.ac.uk/pint/) (Perrin and Schnepp 2004; Biggin et al. 2009; Biggin et al. 2010), which contains data from igneous materials older than 50 ka. In addition, GEOMAGIA50 incorporates relevant data from the PANGAEA database (http://www.pangaea.de) (Diepenbroek et al. 2002), the National Oceanic and Atmospheric Administration (NOAA) National Climatic Data Center (NCDC) paleoclimatology datasets (http://www.ncdc.noaa.gov/data-access/paleoclimatology-data/datasets), the Ocean Drilling Program (ODP) and International Ocean Discovery Program (IODP) Janus database (http://www-odp.tamu.edu/database/), and the SEDPI06 compilation of (Tauxe and Yamazaki 2007), available through entries in the MagIC database. It supersedes the IAGA SECVR00 database (http://www.ngdc.noaa.gov/geomag/paleo.shtml) for lake sediments (McElhinny and Lock 1996), which has not been updated since 1999. All data within SECVR00 will be transferred to GEOMAGIA50 and augmented with additional metadata.
The GEOMAGIA50 database for sediments builds upon the principles described in Korhonen et al. (2008) and Brown et al. (2015) for the GEOMAGIA50 database for archeological and volcanic materials. The structure of the database (see the ‘Sediment database structure’ section and the ‘Data types’ section) has been significantly expanded to accommodate the greater diversity of magnetic measurements made on lake and marine sediments and the large number of dating methods applicable. The web query form is hosted at http://geomagia.gfz-potsdam.de/geomagiav3/SDquery.php and mirrored at http://geomagia.ucsd.edu/.
Sediment database structure
Individual (specimen/stratigraphic) paleomagnetic and rock magnetic results;
Processed (averaged/smoothed) paleomagnetic results;
Reconstructed paleomagnetic data.
These tables are available to download by the user upon querying the database (see the ‘Query results’ section). The rationale behind the results tables is described in the ‘Individual (specimen/stratigraphic) paleomagnetic and rock magnetic data results table’ to ‘Reconstructed paleomagnetic data results table’ sections. Spanning the five results tables are 158 unique fields (258 in total) which are shown in the tables in Additional file 1. Additional file 1: Table S1 lists fields common to at least two results tables. Additional file 1: Tables S2 to S6 document fields unique to particular results tables. A glossary of terms used to describe different aspects of the database can be found in Table one of Brown et al. (2015).
Depth as the common link between data types
Unlike GEOMAGIA50 for archeological and volcanic materials, where data are primarily organized by age, the most important link between results from the same core, or between cores from the same location, is depth. Ideally, the original core depth will be documented. This is the depth before any corrections or correlations to other cores have been made. Data on core depth give the greatest flexibility in reinterpreting the data. However, it is common that data will be given on a composite depth scale (the depth after corrections or correlations). The database accommodates both depth types with separate entries. Reporting on depth allows chronological data to be tied uniquely to magnetic data.
Individual (specimen/stratigraphic) paleomagnetic and rock magnetic data results table
The most fundamental level of data reported is from a specimen or stratum at a specific depth, e.g., a characteristic remanent magnetization (ChRM) direction or a hysteresis parameter. It is the single value an author feels is representative of a given property of the sediment at a specific depth. Unlike the MagIC database (Constable et al. 2006), the individual measurements used to determine this value are not archived. Using again the example of a paleomagnetic direction, the moments of the natural remanent magnetization (NRM) of the sediment at increasing alternating field steps used to calculate the ChRM are not reported. Such data are commonly not available. When they are, the MagIC database is already adequately equipped to store these types of data.
Data at the specimen or stratigraphic level are the building blocks of any time series, and the provision of these data will allow any researcher to create a new, or recreate the original, time series. The entries unique to this table are listed in Additional file 1: Table S2.
The data in a single entry were obtained from the same specimen or layer of sediment, with the exception of data digitized from a publication graphic, where this can often not be uniquely determined (see the ‘Data sources’ section). If two specimens were taken at the same depth, they have separate entries in the database.
Data may be obtained from discrete specimens or from continuous measurements. For discrete measurements, specimens are extracted from the sediment at known spacings. For example, discrete paleomagnetic and rock magnetic measurements are often made on plastic cubes with a small volume; however, their size may vary, and although the length of a side may cover a range of depths, only one depth will be reported in most cases. This may be the depth of the top, middle, or bottom of the specimen depending on a particular researcher’s preference, but this is rarely reported, and this information is therefore not accommodated in the database. Continuous measurements are made on the split half of a core or from a meter-long u-channel extracted from the split half. The sediment is either passed through/under a sensor, or a sensor moves over the sediment. In both cases, measurements will be taken at a set spacing. The independence of an individual measurement depends on the response function of the sensor, whether from a long-core susceptibility meter (see Nowaczyk 2001) or a pass-through cryogenic magnetometer (see Jackson et al. 2010, and reference therein). It would be incorrect to label measurements made on split halves or u-channels as specimen measurements; however, they are measurements made with the central point of the sensor over a stratum with a certain depth. The title of the table aims to reflect these two measurement types.
Processed (averaged/smoothed) paleomagnetic data results table
At the processed level, only paleomagnetic data that have been processed in some way are shown (see Additional file 1: Table S3). As these data have been manipulated, they cannot be linked uniquely to a specific specimen or depth in the individual paleomagnetic and rock magnetic data results table, radiocarbon table, or age table. A variety of statistical approaches have been applied on either composite depth or age scales, e.g., discrete or moving averages, spline fits, or interpolations. If a composite depth is given (see the ‘Depth as the common link between data types’ section), this is not the composite depth of an individual specimen or stratum, but a depth that has been manipulated within the composite depth scale. The scale of smoothing (on depth or time), the number of specimens/strata used for the averaging or smoothing of each value (N specimens), and the method of averaging or smoothing are reported (for directions: Dir. Smoothing Type ID; for relative paleointensity: RPI Smoothing Type ID).
Averaged/smoothed data have commonly been ‘stacked’ together from multiple cores and then processed. In the case where data have been stacked, but not processed, the composite depth has not been manipulated, and no core identifier exists; the data are recorded in the individual paleomagnetic and rock magnetic data results table. They are labeled ‘Stack’ under ‘Core ID’.
Radiocarbon ages and general ages results tables
Chronological data have been split into two results tables: radiocarbon ages and general ages. This is purely for practical reasons. The number of different experimental details related to radiocarbon measurements and ages determined using other methods (see the ‘Chronological data’ section) would make the online output table prohibitively large if combined. The entries unique to these tables are listed in Additional file 1: Table S4 and Table S5.
Reconstructed paleomagnetic data results table
An important objective of the database is to allow users to recreate an original paleomagnetic time series or create a new time series from data documented in the individual paleomagnetic and rock magnetic data results table and chronological results tables. It may be desirable to construct a new time series when additional data subsequent to the original time series’ publication become available. Research on a location may continue for a number of years after the original publication or a location may be revisited at a later date. For example, the original paleosecular variation data from Lake Keilambete, Australia, was published by Barton and McElhinny (1981); however, the lake was revisited by Wilkins et al. (2012), who obtained additional chronological data from a newly drilled core. We have reconstructed this record by creating a new time scale using a combination of radiocarbon ages (Bowler and Hamada 1971; De Deckker 1982; Dodson 1974; Polach and Barton 1983; Wilkins et al. 2012; Yamasaki et al. 1970) and optically stimulated luminescence ages (Wilkins et al. 2012) and applied the Bayesian age-depth modeling algorithm of Blaauw and Christen (2011) to generate a new age-depth model with age uncertainties. This example series is available within the database.
We assign a separate results table for reconstructed time series. This is to distinguish our interpretation of the data from the data of the original studies. The database will be updated with reconstructed time series on their publication. The entries unique to this table are listed in Additional file 1: Table S6.
Metadata tables and identification numbers
A variety of approaches are taken in acquiring the majority of data types. It is therefore necessary to fully report, e.g., experimental methods, data processing procedures, or materials used in the results tables (see the ‘Individual (specimen/stratigraphic) paleomagnetic and rock magnetic data results table’ to ‘Reconstructed paleomagnetic data results table’ sections). Owing to the large nature of the database, a series of identification numbers (IDs) have been employed to accommodate these metadata. IDs are linked to a description of the accompanying data through 33 metadata relational tables. Metadata tables can be utilized by more than one of the results tables, e.g., error types. The relationship between the results tables and the metadata tables is described fully in Brown et al. (2015). In the online table visible to the user after querying (see the ‘Query results’ section), the ID related to a specific data entry is shown in an output field next to the data, and the ID is described in a relational table below the main results table.
A useful application of a metadata relational table is in the identification of curves used to calibrate radiocarbon ages for variations in atmospheric carbon through time. Different atmospheric radiocarbon calibration curves have been developed for northern and southern hemispheres and for marine and terrestrial environments. These curves have been refined through time (see Clark 1979 and Reimer et al. 2013). It is important to note which calibration curve was used in a particular study, as although applicable at the time of publication, it may have been superseded. Recalibration can result in a revision of ages used in the transfer of depth to age and a subsequent modification of paleomagnetic and rock magnetic time series.
Rock magnetic data;
As individual studies are conducted with specific aims in mind, the types of data reported in each study may vary and some may contain a measurement type or variable determination unique to that study. It is not practical to report every type of data. We have chosen data types that appear generally representative of those collected in sedimentary magnetism.
Paleomagnetic data are primarily ChRM directions (inclinations and declinations) and relative paleointensity (RPI). These data often undergo different types of corrections or processing and may be reported in the literature at one or more processing steps. The database includes a variety of information about these processing steps.
At the individual (specimen/stratigraphic) level, two sets of inclinations and declinations are accommodated. First are directions before any correction or processing. They are labeled Dec raw and Inc raw. They are accompanied by an entry for the maximum angular deviation (MAD) if the ChRM direction was calculated using principal component analysis (Kirschvink 1980). Secondly, declinations and inclinations may be corrected for imperfections in the coring process. The database contains corrected declinations (Dec adj) and inclinations (Inc adj) and information on the methods of adjustment. The IDs for the types of adjustments are shown in two fields (Dec adj ID and Inc adj ID) and are linked to a metadata table describing the IDs.
It is common for cores not to be oriented in the horizontal plane. Assumptions of the field behavior over the length of the core are required to produce declination records that appear geophysically reasonable. One approach is to assume that the geomagnetic field tends to a geocentric axial dipole (GAD) over the time covered by the length of the core. All declinations are rotated so the mean or median declination is zero degrees. A second less commonly used approach is to match a portion of a declination record with contemporaneous historical observations. For example, the declination record of Lake Pounui, New Zealand (Turner and Lillis 1994), was rotated so the upper portion of the core matched the historical observations of Abel Tasman. In addition, cores may become twisted on extraction. This can result in a progressive rotation of the declination record with depth. In some cases, authors attempt to recover the declination by removal of a pervasive trend.
Sub-vertical coring may steepen or shallow inclinations. Different approaches have been taken in attempts to restore reliable inclinations. For example, as with declination, if a GAD field is assumed, all inclinations can be rotated so their mean has the expected inclination for the sampling latitude.
For the above adjustment procedures, declination and inclination have been treated separately. However, methods have been proposed to vectorially align declination and inclination to either a master record (no or minimal distortions are assumed) (e.g., Denham 1981; McFadden 1982) or to the GAD field (e.g., Turner and Thompson 1981).
At the processed level, only one set of directional values are reported, and these are the final time series preferred by the author. As with individual data, the methods of adjustments are reported (Dec ID and Inc ID). Directional uncertainties are recorded as σ Dec and σ Inc. The type of uncertainty is shown under σ ID. If uncertainty is given as α 95 (Fisher 1953), σ Dec is shown as (81/140cos(I)) α 95 where I = inclination; σ Inc is reported as (81/140) α 95 (Piper 1989).
To calculate an RPI, the NRM of a sediment must be normalized to compensate for changes in the concentration of magnetic minerals within the sediment. Any normalizer must activate the same population of magnetic grains that carry the NRM. This is most crudely achieved by dividing an NRM by an anhysteretic remanent magnetization (ARM), an isothermal remanent magnetization (IRM), or susceptibility (k). See King et al. (1983), Roberts et al. (2013), Tauxe (1993), Tauxe and Yamazaki (2007), and Valet (2003) for more detailed discussion on the methodologies and caveats regarding the calculation of RPI.
At both the individual data level and processed data level, NRM/ARM, NRM/IRM, and NRM/k are accommodated. In a few studies, RPI has been converted to a virtual dipole moment (VDM) or a virtual axial dipole moment (VADM) (e.g., Peck et al. 1996), and we additionally include VDM and VADM as a single field. As the instances where VDM or VADM are reported are few, the reader is referred to individual publications for details on how the RPI data were calibrated. An author’s preferred method of normalization is shown in RPI pref ID. If an author does not have a preferred normalizer, then all methods are shown. In some cases, RPI values have been normalized around zero mean. These data are flagged under RPI pref ID.
The NRM/ARM and NRM/IRM entries accommodate values calculated with a variety of methods: NRM/ARM or NRM/IRM at a specific AF step (Levi and Banerjee 1976), a mean of multiple NRM/ARM or NRM/IRM values at a range of AF steps (Channell et al. 1997), a linear fit through NRM and ARM or IRM values at different AF steps (e.g., Channell et al. 2012; Nowaczyk et al. 2013), vector-subtracted NRM/ARM or NRM/IRM (Channell et al. 2000), and the pseudo-Thellier method (Tauxe et al. 1995). The NRM, k, ARM, and IRM values used in the calculation of RPI are also reported (e.g., NRM rpi) along with an indication of an author’s preferred normalization method (RPI pref), if noted. Uncertainties on RPI measurements include the standard error on least squares fits to NRM/ARM or NRM/IRM across a range of AF steps, the standard deviation on the mean of multiple NRM/ARM or NRM/IRM values at a range of AF steps, or the standard deviation of multiple RPI values across a range of depths or times.
Rock magnetic data
A large variety of rock magnetic parameters and ratios are documented in the database (see Additional file 1: Table S2). These data are often used to assess the concentration, grain size, and mineralogy of magnetic minerals contained within sediments (see Liu et al. 2012; Verosub and Roberts 1995) and can help identify oxidation, dissolution, and growth of new magnetic minerals (e.g., Nowaczyk 2011). The magnetic properties of sediments and their variation through time can reflect changes in environment or climate (Liu et al. 2012) and are essential for assessing the reliability of RPI records (King et al. 1983; Tauxe 1993; Tauxe and Yamazaki 2007). RPI is notoriously difficult to obtain and can often be contaminated by lithological variations induced by environmental changes (e.g., Guyodo et al. 2000; Haltia-Hovia et al. 2011; Stanton et al. 2011; Valet et al. 2011; Yamazaki et al. 2013) or by factors yet unknown (Tauxe and Yamazaki 2007). To develop a greater understanding of the evolution of the geomagnetic field through time, the influence of the magnetic properties of sediments on RPI must be more fully understood.
The physical processes responsible for the acquisition of remanence in sediments are poorly understood (see reviews by Roberts et al. 2013 and Tauxe 1993 and within Heslop et al. 2014). Along with the simulation of deposition conditions and remanence acquisition through laboratory experiments (e.g., Carter-Stiglitz et al. 2006; Katari et al. 2000; Lu et al. 1990; Spassov and Valet 2012; Tucker 1981; van Vreumingen 1993) and modeling (e.g., Heslop et al. 2014; Katari and Bloxham 2001; Mitra and Tauxe 2009; Nagata 1961; Roberts and Winklhofer 2004; Tauxe et al. 2006) the substantial amount of rock magnetic data coupled with paleomagnetic data can identify whether there are any specific relationships between the two that may be linked to the remanence acquisition process. We have documented rock magnetic parameters that are consistently reported in the literature but acknowledge that more detailed experimental measurement level data from, e.g., hysteresis, first-order reversal curve (FORC), stepwise ARM, and IRM acquisition and demagnetization measurements, would allow the greatest flexibility in the investigation of the remanence acquisition process. However, these data are not currently included in GEOMAGIA50 (see the ‘Individual (specimen/stratigraphic) paleomagnetic and rock magnetic data results table’ section). Such data are more easily accommodated in the MagIC database, but at the moment, there are none from sediments deposited over the past 50 ka.
An emphasis has been placed on comprehensively reporting chronological information and the methods used to transfer depth to age. Radiocarbon, oxygen isotope, varve, tephra, 137Cs and 210Pb ages, and their metadata are accommodated in the database. These data are contained within two output tables: (1) Radiocarbon Age Tables and (2) General Age Tables (see the ‘Sediment database structure’ section). Experimental details, materials, and in the case of radiocarbon ages, details of the calibration curves (Calib. dataset ID) and software (Calib. software ID) used to correct for variations in 14C in atmospheric CO 2 through time are all documented in the database. A complete list of entries are shown in Additional file 1: Table S4 and Table S5. Details of the age-depth models used to create time series are documented in the individual and processed data tables and shown under the Age-Depth Model ID heading (Additional file 1: Table S1). For chronological data, the uncertainty is commonly an experimental error given as a standard deviation or a range of ages, e.g., after calibration of radiocarbon ages.
Metadata are descriptive data applicable to (1) the sedimentary setting (e.g., location name, coordinates, or depositional environment); (2) the paleomagnetic, rock magnetic, and chronological data (e.g., measurement and analysis methods, types of specimens); (3) publications and data sources; and (4) entry of data to the database (date and person responsible for uploading data). For (2), metadata are listed alongside the values for a certain parameter and in the majority of cases are an ID (see tables in Additional file 1).
Every entry in the database is accompanied by at least one ‘Reference ID.’ The data at a specific depth or time may be described in multiple publications or different data types may have been published in different articles, e.g., paleomagnetic, rock magnetic, and chronological data, such as for Birkat Ram, Israel (Frank et al. 2002; 2003; Schwab et al. 2004). To overcome a technical limitation with how references are stored within the database, a reference, or a set of references, are given what we term a ‘Reference Group ID.’ For the Birkat Ram example, ‘Reference ID’ 44 to 46 are grouped under ‘Reference Group ID’ 9. A full list of references, including the ‘Reference Group ID’ and ‘Reference ID’ is available on an accompanying web page (http://geomagia.gfz-potsdam.de/sedimentstudies.php), which is accessible through the left navigation menu (Additional file 1: Section 1.2). References include a DOI or a hyperlink to a permanent holding.
The date of upload acts as a version marker. If data are amended or appended, the date of upload will be modified. The initials of the person responsible for the upload of the data are shown under ‘Uploader.’ The name and email details of the person responsible for the upload are listed in a relational table below the relevant results table. Users are encouraged to contact the uploader if mistakes are found with any of the data.
Reporting uncertainties is crucial for the assessment and creation of any time series. This is particularly true for paleosecular variation time series from sediments, where there are non-trivial uncertainties in both chronological and paleomagnetic data (Nilsson et al. 2014; Panovska et al. 2012). Global models of the geomagnetic field and interpretation of other time series are hindered by the under reporting of age uncertainties and the variety of approaches used to transfer depth to age. Age uncertainties were not included in the individual models of the CALSxk series of models (e.g., (e.g., Korte et al. 2011), and they were set to a fixed value (±300 years) in the bootstrap method applied to generate average models with uncertainty limits. In the pfm9k.1a global geomagnetic field model of Nilsson et al. (2014), paleomagnetic time series were temporally aligned to a preliminary global model within a set ±500-years limit. It would be desirable to incorporate more rigorously determined chronological uncertainties, related to the measurement and calibration procedure of radiocarbon ages or other age data, into future global field models. To accommodate such approaches, the database contains detailed information on paleomagnetic and chronological uncertainties and experimental details. This will allow any researcher to construct new age-depth models and time series for a specific location. It will also allow a consistent methodology to be used when creating a suite of age-depth models from different locations.
The type of uncertainty may differ with the kind of measurement, and between studies different types of uncertainties may be reported for the same data type. We document uncertainties and their type with each measurement, where these data are available.
Data reporting and units
Data values and units are those published. However, if values are too small or too large to be conveniently written in decimal form, they have been placed in standard scientific notation (magnetization and susceptibility may span many orders of magnitude). Fields titled ‘Factor’ list the base and its exponent as published or as adjusted by us. ‘Unit’ fields list published units. ‘Factor’ and ‘Unit’ fields accompany all rock magnetic values, namely susceptibility, NRM, ARM, IRM, HIRM, and hysteresis data, as SI and cgs unit systems are used in the literature and susceptibility and magnetization maybe be normalized by volume, mass, or not normalized. In some cases, units are not documented. Ideally, standardized factors and units would be reported in the database; however, the range of factors and the use of different units for the same parameters make it difficult to transform units. In a number of cases, transformation would require the mass or volume of each specimen to be reported. This is rarely done.
In comparison with the GEOMAGIA50 database for archeomagnetic and volcanic data, where ages are reported in years AD, all sediment age constraints and output are shown in years before present (yr. BP), where present is defined as 1950 AD. This is to be consistent with the standard zero year used in radiocarbon dating. The majority of sediment ages are reported in yr. BP or ka, which are equivalent.
At the time of writing, approximately 300 studies have reported paleomagnetic results from over 700 lacustrine and marine cores covering at least some part of the past 50 ka. The large number of studies means population of the database must be ongoing. Legacy data and data from new studies will be incorporated into the database as we acquire them.
an author directly,
a table in a publication or supplementary material,
another database (e.g., SECRV00, PANGAEA, NOAA/NCDC, Janus or MagIC),
digitization of published graphic material.
The sources of the data are shown under the ‘Source ID’ entries in the results and metadata tables generated on querying the database. Data obtained from authors, publication tables and supplementary materials, or other databases are most reliable. Close communication with authors provides the most accurate reproduction of the data that appear in a publication. We have endeavored to provide the full data set as described in a publication.
Data from older publications are often not available in digital form; however, they can be digitized. These data are valuable for expanding the number of paleomagnetic measurements that can be used in global modeling of the geomagnetic field. However, caution must be exercised when using digitized data, as values cannot be precisely determined. Small uncertainties on digitized depth or age mean that although data can be from the same specimen or stratum, when parameters are digitized from different graphs (e.g., inclination and declination are shown on separate axes), it is not possible to unequivocally link data to the same specimen/stratum. This is common when data are closely spaced in depth or time or if two discrete specimens were measured at the same depth. To be conservative, each digitized datum is assigned a unique depth or age.
We have developed a digitization algorithm for pixel-based graphics using MATLAB. All digitized data in the database were obtained using this method. The algorithm considers rotation and distortion of the image. In some cases, axes are not precisely orthogonal, or the page is rotated. This is common for older articles where graphics have been scanned by us or a publisher. Automatic and manual data recognition are accommodated. Automatic data recognition is preferred where possible as it reduces the subjectivity associated with the manual selection of data. To estimate the deviation of manually defined points from their true coordinates, we digitized a graph of 100 randomly generated points with known coordinates at six levels of zoom. For these 600 points the mean deviation was 1.8%.
We encourage the scientific community to help in the population of the database by including data at the specimen/stratum level and averaged/smoothed level as Additional file 1 when publishing, following a table structure similar to that of the GEOMAGIA50.CSV output files (see the ‘Query results’ section).
Global models of the Holocene geomagnetic field
Unlike for archeo/volcanic queries (Brown et al. 2015), model predictions are not plotted, as the variety of parameters which could be plotted on different depth scales and age scales, and the large amount of data available for some locations, would greatly increase the time required to process each query. They are available for download only. See Brown et al. (2015) for descriptions of the column headers used in the model output files.
User interface: GEOMAGIA50 web page
Sediment query form
Query, download and model options;
Advanced querying options;
These options are described in the following sections. A user’s guide to operating the query form is given in Additional file 1.
Query, download and model options
Individual (specimen/stratigraphic) data,
Processed (averaged/smoothed) data,
Reconstructed paleomagnetic data are automatically queried when either ‘Individual (specimen/stratigraphic) data’ or ‘Processed (averaged/smoothed) data’ are selected. ‘Model options,’ allows the user to query temporally continuous spherical harmonic models of the Holocene geomagnetic field (see the ‘Global models of the Holocene geomagnetic field’ section).
Data between 50 ka and the present can be queried, and the user can select all or part of this time interval (Figure 5). If no age constraints are selected, then data that are only on depth can also be retrieved (see Additional file 1: Section 1.1.2). This will be common for individual data from specific cores, as these data are often reported prior to application of an age-depth model. Age constraints are shown in years BP.
A great deal of flexibility in querying is provided within geographic constraints. The user can choose no geographic constraints (useful for global searches of specific data types, see the‘Advanced querying options’ section) through to selecting data from a specific core (Figure 5 and Additional file 1: Section 1.1.3).
A significant portion of magnetic data from sediments from the past 50 ka come from marine cores. As marine cores are more commonly known by their location and core names (e.g., IODP, ODP, and MD site numbers), a dedicated field to search by core name has been included.
Advanced querying options
Individual data choices are split into three primary categories: directional, RPI, and rock magnetic data (Figure 6). These splits are motivated by current research interests within paleomagnetism and rock magnetism. For example, RPI data alone can be used to improve our understanding of the paleomagnetic power spectrum (Figure 1), and compilations of RPI data have been used to construct global and regional paleointensity stacks to aid in stratigraphic studies and to help in defining the global character of the geomagnetic field (see the ‘Introduction’ section). Being able to filter out studies with no RPI data greatly increases the efficiency of these types of analyzes.
Environmental or climate studies may not require paleomagnetic data, with the exception of those using paleomagnetic dating to infer the timing of environmental or climate changes (e.g., Stott et al. 2002). Researchers may be interested in investigating certain parameters; therefore, searches for rock magnetic data can be further refined. More than one rock magnetic parameter can be queried at once (Figure 6b). The database returns entries that contain at least one of the rock magnetic parameters checked (‘or’ statements), e.g., if ‘Hysteresis parameters’ and ‘S-ratio or HIRM’ are selected, entries will be returned that contain either hysteresis or S-ratio/HIRM data. It does not limit the entries that are returned to those containing both hysteresis and S-ratio/HIRM data solely. This allows the user to view the complete entry for a specimen or horizon that contains the parameter(s) of interest. A range of data types are often used in combination to determine magnetic grain size and mineralogy. It is therefore advantageous to view all complementary data.
The choice of ‘General age data’ to be queried can also be refined (Figure 6). As with the rock magnetic parameters, multiple general age constraints can be queried at once.
The column headers shown online and in the.CSV files are described in Additional file 1: Tables S1 to S6. Within the tables, the ordering of entries is governed sequentially, first by ‘Location Code’ (in alphabetical order), then ‘Core ID’ (in alphabetical order), ‘Core Depth (cm)’ or ‘Composite Depth (cm)’ (depending on which is given; however, if both exist, data will be arranged by core depth), and finally ‘Age (yr. BP)’. Above the results tables, summaries of the query parameters chosen by the user are displayed (Figure 8).
Each table contains a number of fields that list the IDs (see the ‘Metadata tables and identification numbers’ section), e.g., the references (Figure 8). Each ID is a hyperlink. On clicking a hyperlink, the page scrolls down to a relational table describing the ID (Figure 8). The relational tables (see the ‘Metadata tables and identification numbers’ section) are found beneath the results table (Figure 8).
If no constraints are selected, then the user is redirected to the web page ‘Complete sediment data sets.’ This page contains hyperlinks to pre-prepared.CSV files with the complete data from the five results tables. At the time of writing, the number of data entries exceeds 30,000, with multiple data available for each entry. Such a large amount of data takes a prohibitively long time to print to the screen. To further reduce the execution time of the query, we limit the output printed to the screen to the first 10 entries that match the constraints specified by the user (all data matching the specified constraints are written to the file).
The GEOMAGIA50 database for sediments is an expansion of the GEOMAGIA50 database, which previously housed only magnetic data from archeological and volcanic materials (Brown et al. 2015; Donadini et al. 2006; Korhonen et al. 2008). The database accommodates paleomagnetic, rock magnetic, radiocarbon, and other age data obtained from marine and lake sediments deposited over the past 50 ka. Data from sediments help constrain interpretations of past changes in the geomagnetic field, the environment, and climate. We document in detail radiocarbon age data, as well as 210Pb, 137Cs, δ 18O, varve, and tephra age information. For all data types, uncertainties are reported where possible.
The database can be accessed through a web query form, which can be found at http://geomagia.gfz-potsdam.de/geomagiav3/SDquery.php and is mirrored at http://geomagia.ucsd.edu/. The interface has been designed to allow rapid selection of data by age, geographic, and data type constraints. More advanced queries based upon specific paleomagnetic, rock magnetic, and chronological types are accommodated. This enables global comparisons of specific data types. The results of queries can be viewed online and downloaded as.CSV files. In addition, users can generate Holocene geomagnetic field model predictions from the CALSxk and pfm9k.1a series of models (e.g., Korte and Constable 2011; Nilsson et al. 2014) for the coordinates used for the data search. These data can be downloaded as.TXT files.
Owing to the large amount of data available from sediments, approximately 300 studies report results from over 700 sediment cores, the uploading of material is ongoing. In addition, new data are frequently obtained from sediments, and the database will be updated as these are published.
Availability and requirements
We kindly thank those who provided data in a digital form. Lisa Tauxe is thanked for providing her SEDPI06 data compilation. MCB, MK, and MS were supported by Deutsche Forschungsgemeinshcaft (DFG) SPP PlanetMag 1488 projects (KO2870/4-1, BR4697/1 and WA2605/2). FD acknowledges the support of the Swiss National Science Foundation (project numbers 130147 and 144102). AN was funded by the Natural Environment Research Council (NE/I013873/1) and the Swedish Research Council (Dnr 2014-4125). SP was funded by US National Science Foundation NSF grant EAR 1246826. CGC gratefully acknowledges support from the Alexander von Humboldt Foundation and US National Science Foundation Grant NSF EAR 12225364. Gesa Petersen is thanked for uploading a substantial amount of data to the database. Two anonymous reviewers are thanked for their comments.
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